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overflow: hidden; text-overflow: ellipsis; -webkit-line-clamp: 3; -webkit-box-orient: vertical; }</style><div class="col-xs-12 clearfix"><div class="u-floatLeft"><h1 class="PageHeader-title u-m0x u-fs30">Habitable Exoplanets</h1><div class="u-tcGrayDark">294 Followers</div><div class="u-tcGrayDark u-mt2x">Recent papers in <b>Habitable Exoplanets</b></div></div></div></div></div></div><div class="TabbedNavigation"><div class="container"><div class="row"><div class="col-xs-12 clearfix"><ul class="nav u-m0x u-p0x list-inline u-displayFlex"><li class="active"><a href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Top Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Habitable_Exoplanets/MostCited">Most Cited Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Habitable_Exoplanets/MostDownloaded">Most Downloaded Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Habitable_Exoplanets/MostRecent">Newest Papers</a></li><li><a class="" href="https://www.academia.edu/People/Habitable_Exoplanets">People</a></li></ul></div><style type="text/css">ul.nav{flex-direction:row}@media(max-width: 567px){ul.nav{flex-direction:column}.TabbedNavigation li{max-width:100%}.TabbedNavigation li.active{background-color:var(--background-grey, #dddde2)}.TabbedNavigation li.active:before,.TabbedNavigation li.active:after{display:none}}</style></div></div></div><div class="container"><div class="row"><div class="col-xs-12"><div class="u-displayFlex"><div class="u-flexGrow1"><div class="works"><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_78786377" data-work_id="78786377" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/78786377/UV_habitable_zones_around_M_stars">UV habitable zones around M stars</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">During the last decade, there was a paradigm-shift in order to consider terrestrial planets within liquid-water habitable zones (LW-HZ) around M stars, as suitable places for the emergence and evolution of life. Here we analyze the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_78786377" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">During the last decade, there was a paradigm-shift in order to consider terrestrial planets within liquid-water habitable zones (LW-HZ) around M stars, as suitable places for the emergence and evolution of life. Here we analyze the influence of UV boundary conditions to three planetary systems around dM (HIP 74995, HIP 109388 and HIP 113020). We apply our model of UV habitable zone (UV-HZ) (Buccino et al. 2006) to these cases and show that during the quiescent UV output there would not be enough UV radiation within the LW-HZ in order to trigger biogenic processes. We also analyze the cases of two other M flare stars and show that the flares of moderate intensity could provide the necessary energy to trigger those biogenic processes, while the strong flares not necessary rule-out the possibility of life-bearing planets.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/78786377" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="a3fa069b16fa267e5f951cef20be3afa" rel="nofollow" data-download="{"attachment_id":85708553,"asset_id":78786377,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/85708553/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="31221696" href="https://ajitha.academia.edu/GuillermoLemarchand">Guillermo A . Lemarchand</a><script data-card-contents-for-user="31221696" type="text/json">{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}</script></span></span></li><li class="js-paper-rank-work_78786377 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="78786377"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 78786377, container: ".js-paper-rank-work_78786377", }); });</script></li><li class="js-percentile-work_78786377 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 78786377; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_78786377"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_78786377 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="78786377"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 78786377; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=78786377]").text(description); $(".js-view-count-work_78786377").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_78786377").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="78786377"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">20</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="407" href="https://www.academia.edu/Documents/in/Geochemistry">Geochemistry</a>, <script data-card-contents-for-ri="407" type="text/json">{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="409" href="https://www.academia.edu/Documents/in/Geophysics">Geophysics</a>, <script data-card-contents-for-ri="409" type="text/json">{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="498" href="https://www.academia.edu/Documents/in/Physics">Physics</a>, <script data-card-contents-for-ri="498" type="text/json">{"id":498,"name":"Physics","url":"https://www.academia.edu/Documents/in/Physics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a><script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=78786377]'), work: {"id":78786377,"title":"UV habitable zones around M stars","created_at":"2022-05-08T15:33:15.424-07:00","url":"https://www.academia.edu/78786377/UV_habitable_zones_around_M_stars?f_ri=334552","dom_id":"work_78786377","summary":"During the last decade, there was a paradigm-shift in order to consider terrestrial planets within liquid-water habitable zones (LW-HZ) around M stars, as suitable places for the emergence and evolution of life. Here we analyze the influence of UV boundary conditions to three planetary systems around dM (HIP 74995, HIP 109388 and HIP 113020). We apply our model of UV habitable zone (UV-HZ) (Buccino et al. 2006) to these cases and show that during the quiescent UV output there would not be enough UV radiation within the LW-HZ in order to trigger biogenic processes. We also analyze the cases of two other M flare stars and show that the flares of moderate intensity could provide the necessary energy to trigger those biogenic processes, while the strong flares not necessary rule-out the possibility of life-bearing planets.","downloadable_attachments":[{"id":85708553,"asset_id":78786377,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}],"research_interests":[{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=334552","nofollow":false},{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false},{"id":498,"name":"Physics","url":"https://www.academia.edu/Documents/in/Physics?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":46818,"name":"Exobiology","url":"https://www.academia.edu/Documents/in/Exobiology?f_ri=334552"},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552"},{"id":49201,"name":"Life in the Universe","url":"https://www.academia.edu/Documents/in/Life_in_the_Universe?f_ri=334552"},{"id":65140,"name":"Models","url":"https://www.academia.edu/Documents/in/Models?f_ri=334552"},{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=334552"},{"id":129770,"name":"Key words","url":"https://www.academia.edu/Documents/in/Key_words?f_ri=334552"},{"id":165671,"name":"Astronomía","url":"https://www.academia.edu/Documents/in/Astronom%C3%ADa?f_ri=334552"},{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":409626,"name":"Intensity","url":"https://www.academia.edu/Documents/in/Intensity?f_ri=334552"},{"id":517654,"name":"Icarus","url":"https://www.academia.edu/Documents/in/Icarus?f_ri=334552"},{"id":548206,"name":"Flare Stars","url":"https://www.academia.edu/Documents/in/Flare_Stars?f_ri=334552"},{"id":1131312,"name":"Academic","url":"https://www.academia.edu/Documents/in/Academic?f_ri=334552"},{"id":1282080,"name":"Terrestrial Planets","url":"https://www.academia.edu/Documents/in/Terrestrial_Planets?f_ri=334552"},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4174128" data-work_id="4174128" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4174128/An_Estimate_of_the_Prevalence_of_Biocompatible_and_Habitable_Planets">An Estimate of the Prevalence of Biocompatible and Habitable Planets</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">A Monte Carlo computer model of extra-solar planetary formation and evolution, which includes the planetary geochemical carbon cycle, is presented. The results of a run of one million galactic disc stars are shown where the aim was to... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4174128" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">A Monte Carlo computer model of extra-solar planetary formation and evolution, which includes the planetary geochemical  carbon cycle, is presented. The results of a run of one million galactic disc stars are shown where the aim was to assess the possible abundance of both biocompatible and habitable planets. (Biocompatible planets are defined as worlds where the long-term presence of surface liquid water provides environmental conditions suitable for the origin and evolution of life. Habitable planets are those worlds with more specifically Earth-like conditions.) The model gives an estimate of 1 biocompatible planet per 39 stars, with the subset of habitable planets being much rarer at 1 such planet per 413 stars. The nearest biocompatible planet may thus lie ~ 14 LY distant and the nearest habitable planet ~ 31 LY away. If planets form in multiple star systems then the above planet/star ratios may be more than doubled. By applying these results to stars in the solar neighbourhood, it is possible to identify 28 stars at distances of < 22 LY with a non-zero probability of possessing a biocompatible planet.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4174128" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="ebb5430b201e00abb7113cad3b285814" rel="nofollow" data-download="{"attachment_id":31676540,"asset_id":4174128,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31676540/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4174128 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4174128"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4174128, container: ".js-paper-rank-work_4174128", }); });</script></li><li class="js-percentile-work_4174128 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4174128; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4174128"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4174128 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4174128"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4174128; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4174128]").text(description); $(".js-view-count-work_4174128").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4174128").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4174128"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="41236" href="https://www.academia.edu/Documents/in/Extrasolar_planets">Extrasolar planets</a>, <script data-card-contents-for-ri="41236" type="text/json">{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="194384" href="https://www.academia.edu/Documents/in/Planet_Formation">Planet Formation</a><script data-card-contents-for-ri="194384" type="text/json">{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4174128]'), work: {"id":4174128,"title":"An Estimate of the Prevalence of Biocompatible and Habitable Planets","created_at":"2013-08-05T02:03:34.217-07:00","url":"https://www.academia.edu/4174128/An_Estimate_of_the_Prevalence_of_Biocompatible_and_Habitable_Planets?f_ri=334552","dom_id":"work_4174128","summary":"A Monte Carlo computer model of extra-solar planetary formation and evolution, which includes the planetary geochemical carbon cycle, is presented. The results of a run of one million galactic disc stars are shown where the aim was to assess the possible abundance of both biocompatible and habitable planets. (Biocompatible planets are defined as worlds where the long-term presence of surface liquid water provides environmental conditions suitable for the origin and evolution of life. Habitable planets are those worlds with more specifically Earth-like conditions.) The model gives an estimate of 1 biocompatible planet per 39 stars, with the subset of habitable planets being much rarer at 1 such planet per 413 stars. The nearest biocompatible planet may thus lie ~ 14 LY distant and the nearest habitable planet ~ 31 LY away. If planets form in multiple star systems then the above planet/star ratios may be more than doubled. By applying these results to stars in the solar neighbourhood, it is possible to identify 28 stars at distances of \u003c 22 LY with a non-zero probability of possessing a biocompatible planet.","downloadable_attachments":[{"id":31676540,"asset_id":4174128,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_71963943" data-work_id="71963943" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/71963943/Ultraviolet_radiation_constraints_around_the_circumstellar_habitable_zones">Ultraviolet radiation constraints around the circumstellar habitable zones</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between 200-300 nm becomes energetically very damaging to most of the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_71963943" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between 200-300 nm becomes energetically very damaging to most of the terrestrial biological systems. On the other hand, UV radiation is usually considered one of the most important energy source on the primitive Earth for the synthesis of many biochemical compounds and, therefore, essential for several biogenesis processes. In this work, we use these properties of the UV radiation to define the boundaries of an ultraviolet habitable zone. We also analyze the evolution of the UV habitable zone during the main sequence stage of the star. We apply these criteria to study the UV habitable zone for those extrasolar planetary systems that were observed by the International Ultraviolet Explorer (IUE). We analyze the possibility that extrasolar planets and moons could be suitable for life, according to the UV constrains pres...</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/71963943" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="e20a9f6618f6aacff9e927299f8033c3" rel="nofollow" data-download="{"attachment_id":81090454,"asset_id":71963943,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/81090454/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="31221696" href="https://ajitha.academia.edu/GuillermoLemarchand">Guillermo A . Lemarchand</a><script data-card-contents-for-user="31221696" type="text/json">{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}</script></span></span></li><li class="js-paper-rank-work_71963943 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="71963943"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 71963943, container: ".js-paper-rank-work_71963943", }); });</script></li><li class="js-percentile-work_71963943 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 71963943; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_71963943"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_71963943 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="71963943"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 71963943; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=71963943]").text(description); $(".js-view-count-work_71963943").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_71963943").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="71963943"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">20</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="407" href="https://www.academia.edu/Documents/in/Geochemistry">Geochemistry</a>, <script data-card-contents-for-ri="407" type="text/json">{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="409" href="https://www.academia.edu/Documents/in/Geophysics">Geophysics</a>, <script data-card-contents-for-ri="409" type="text/json">{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a><script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=71963943]'), work: {"id":71963943,"title":"Ultraviolet radiation constraints around the circumstellar habitable zones","created_at":"2022-02-20T07:17:37.351-08:00","url":"https://www.academia.edu/71963943/Ultraviolet_radiation_constraints_around_the_circumstellar_habitable_zones?f_ri=334552","dom_id":"work_71963943","summary":"Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between 200-300 nm becomes energetically very damaging to most of the terrestrial biological systems. On the other hand, UV radiation is usually considered one of the most important energy source on the primitive Earth for the synthesis of many biochemical compounds and, therefore, essential for several biogenesis processes. In this work, we use these properties of the UV radiation to define the boundaries of an ultraviolet habitable zone. We also analyze the evolution of the UV habitable zone during the main sequence stage of the star. We apply these criteria to study the UV habitable zone for those extrasolar planetary systems that were observed by the International Ultraviolet Explorer (IUE). We analyze the possibility that extrasolar planets and moons could be suitable for life, according to the UV constrains pres...","downloadable_attachments":[{"id":81090454,"asset_id":71963943,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}],"research_interests":[{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=334552","nofollow":false},{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":46818,"name":"Exobiology","url":"https://www.academia.edu/Documents/in/Exobiology?f_ri=334552"},{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=334552"},{"id":112063,"name":"Uv Radiation","url":"https://www.academia.edu/Documents/in/Uv_Radiation?f_ri=334552"},{"id":137179,"name":"Origin of Life","url":"https://www.academia.edu/Documents/in/Origin_of_Life?f_ri=334552"},{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=334552"},{"id":220059,"name":"Subject headings","url":"https://www.academia.edu/Documents/in/Subject_headings?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":343860,"name":"Planetary system formation","url":"https://www.academia.edu/Documents/in/Planetary_system_formation?f_ri=334552"},{"id":351461,"name":"Biological systems","url":"https://www.academia.edu/Documents/in/Biological_systems?f_ri=334552"},{"id":517654,"name":"Icarus","url":"https://www.academia.edu/Documents/in/Icarus?f_ri=334552"},{"id":531200,"name":"Extraterrestrial Life","url":"https://www.academia.edu/Documents/in/Extraterrestrial_Life?f_ri=334552"},{"id":724456,"name":"Espectroscopía UV","url":"https://www.academia.edu/Documents/in/Espectroscopia_UV?f_ri=334552"},{"id":882081,"name":"Ultraviolet Radiation","url":"https://www.academia.edu/Documents/in/Ultraviolet_Radiation?f_ri=334552"},{"id":1003892,"name":"Energy Source","url":"https://www.academia.edu/Documents/in/Energy_Source?f_ri=334552"},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_44808806" data-work_id="44808806" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/44808806/Application_of_Data_Mining_to_Search_for_Potentially_Habitable_Exoplanets">Application of Data Mining to Search for Potentially Habitable Exoplanets</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Many light years away from our own solar system, over four thousand confirmed planets orbit stars in a fashion similar to our own eight planets and the sun. With the discovery of these planets, called “exoplanets,” comes the question of... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_44808806" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Many light years away from our own solar system, over four thousand confirmed planets orbit stars in a fashion similar to our own eight planets and the sun. With the discovery of these planets, called “exoplanets,” comes the question of extraterrestrial life, a concept scientists have been exploring for years. The possibility of exoplanetary habitability relies on a number of factors, such as spectral type, density, and eccentricity, but most importantly: whether the exoplanet in question contains water, the fundamental requirement for life, as we know it, to exist. To determine whether an exoplanet provides the ideal conditions for sustaining this vital ingredient for life, we considered the concept of the Goldilocks Zone, or the circumstellar habitable zone (CHZ)—the range of orbits around a star where liquid water is capable of existing. The research we have been conducting this summer utilizes the public dataset provided by NASA and Caltech and data mining methods, including Python and Microsoft Excel, to identify exoplanets with potentially habitable conditions. The discovery of the exoplanet K2-18b’s water vapor-containing atmosphere was a major part of our research, in which we focused on identifying exoplanets with similar attributes to that of K2-18b, in hopes that they too may be able to retain atmospheric water vapor. After a two-month period, we discovered that 59 exoplanets orbit in the CHZ of their host star. As for the K2-18b ruleset, only 1 planet, K2-3d, satisfies the conditions. We believe K2-3d to have a high degree of similarity to K2-18b, but more in-depth analysis will have to be conducted to conclude its potential to support atmospheric water vapor and life as we know it.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/44808806" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="ae415c16eabf6aa9dcb8fdac85653496" rel="nofollow" data-download="{"attachment_id":65308366,"asset_id":44808806,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/65308366/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="174030512" href="https://independent.academia.edu/HrithikPai">Hrithik Pai</a><script data-card-contents-for-user="174030512" type="text/json">{"id":174030512,"first_name":"Hrithik","last_name":"Pai","domain_name":"independent","page_name":"HrithikPai","display_name":"Hrithik Pai","profile_url":"https://independent.academia.edu/HrithikPai?f_ri=334552","photo":"https://0.academia-photos.com/174030512/48523259/38495965/s65_hrithik.pai.jpg"}</script></span></span></li><li class="js-paper-rank-work_44808806 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="44808806"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 44808806, container: ".js-paper-rank-work_44808806", }); });</script></li><li class="js-percentile-work_44808806 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 44808806; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_44808806"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_44808806 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="44808806"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 44808806; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=44808806]").text(description); $(".js-view-count-work_44808806").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_44808806").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="44808806"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="2008" href="https://www.academia.edu/Documents/in/Machine_Learning">Machine Learning</a>, <script data-card-contents-for-ri="2008" type="text/json">{"id":2008,"name":"Machine Learning","url":"https://www.academia.edu/Documents/in/Machine_Learning?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="2009" href="https://www.academia.edu/Documents/in/Data_Mining">Data Mining</a>, <script data-card-contents-for-ri="2009" type="text/json">{"id":2009,"name":"Data Mining","url":"https://www.academia.edu/Documents/in/Data_Mining?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="47599" href="https://www.academia.edu/Documents/in/Astronomy">Astronomy</a><script data-card-contents-for-ri="47599" type="text/json">{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=44808806]'), work: {"id":44808806,"title":"Application of Data Mining to Search for Potentially Habitable Exoplanets","created_at":"2020-12-31T09:58:51.459-08:00","url":"https://www.academia.edu/44808806/Application_of_Data_Mining_to_Search_for_Potentially_Habitable_Exoplanets?f_ri=334552","dom_id":"work_44808806","summary":"Many light years away from our own solar system, over four thousand confirmed planets orbit stars in a fashion similar to our own eight planets and the sun. With the discovery of these planets, called “exoplanets,” comes the question of extraterrestrial life, a concept scientists have been exploring for years. The possibility of exoplanetary habitability relies on a number of factors, such as spectral type, density, and eccentricity, but most importantly: whether the exoplanet in question contains water, the fundamental requirement for life, as we know it, to exist. To determine whether an exoplanet provides the ideal conditions for sustaining this vital ingredient for life, we considered the concept of the Goldilocks Zone, or the circumstellar habitable zone (CHZ)—the range of orbits around a star where liquid water is capable of existing. The research we have been conducting this summer utilizes the public dataset provided by NASA and Caltech and data mining methods, including Python and Microsoft Excel, to identify exoplanets with potentially habitable conditions. The discovery of the exoplanet K2-18b’s water vapor-containing atmosphere was a major part of our research, in which we focused on identifying exoplanets with similar attributes to that of K2-18b, in hopes that they too may be able to retain atmospheric water vapor. After a two-month period, we discovered that 59 exoplanets orbit in the CHZ of their host star. As for the K2-18b ruleset, only 1 planet, K2-3d, satisfies the conditions. We believe K2-3d to have a high degree of similarity to K2-18b, but more in-depth analysis will have to be conducted to conclude its potential to support atmospheric water vapor and life as we know it.","downloadable_attachments":[{"id":65308366,"asset_id":44808806,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":174030512,"first_name":"Hrithik","last_name":"Pai","domain_name":"independent","page_name":"HrithikPai","display_name":"Hrithik Pai","profile_url":"https://independent.academia.edu/HrithikPai?f_ri=334552","photo":"https://0.academia-photos.com/174030512/48523259/38495965/s65_hrithik.pai.jpg"}],"research_interests":[{"id":2008,"name":"Machine Learning","url":"https://www.academia.edu/Documents/in/Machine_Learning?f_ri=334552","nofollow":false},{"id":2009,"name":"Data Mining","url":"https://www.academia.edu/Documents/in/Data_Mining?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4173808" data-work_id="4173808" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4173808/Extra_Solar_Planetary_Systems_A_Microcomputer_Simulation">Extra-Solar Planetary Systems: A Microcomputer Simulation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">""Knowledge of the physical and chemical processes which occur within the circum-stellar nebula of a newly formed star is still uncertain and permits a number of distinct theories to account for the formation of planets. In order to gain... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4173808" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">""Knowledge of the physical and chemical processes which occur within the circum-stellar nebula of a newly formed star is still uncertain and permits a number of distinct theories to account for the formation of planets. In order to gain a greater insight into the complexities of planetary formation, researchers have concentrated on 'realistic' simulations of clearly defined and limited aspects of the problem of the formation of the Solar System. Attempts to describe the nature of planetary systems of other stars have been left largely to popular speculation. <br />The microcomputer model presented here produces a wide range of data for possible planetary systems with primary stars in the mass range 0.6 - 1.3 M⊙. A synthesis of current theory, research and speculation, the purpose of this model is not to add to our understanding of the processes that form planets, but to give an integrated view of the possible nature of extra-solar planetary systems and to investigate the possibility of a systematic variation in planetary characteristics with primary mass. ""</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4173808" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="1d1ac6f02a7dbbb3364587c0f9376b5a" rel="nofollow" data-download="{"attachment_id":31676329,"asset_id":4173808,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31676329/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4173808 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4173808"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4173808, container: ".js-paper-rank-work_4173808", }); });</script></li><li class="js-percentile-work_4173808 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4173808; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4173808"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4173808 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4173808"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4173808; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4173808]").text(description); $(".js-view-count-work_4173808").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4173808").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4173808"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="41236" href="https://www.academia.edu/Documents/in/Extrasolar_planets">Extrasolar planets</a>, <script data-card-contents-for-ri="41236" type="text/json">{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="194384" href="https://www.academia.edu/Documents/in/Planet_Formation">Planet Formation</a>, <script data-card-contents-for-ri="194384" type="text/json">{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4173808]'), work: {"id":4173808,"title":"Extra-Solar Planetary Systems: A Microcomputer Simulation","created_at":"2013-08-05T01:10:05.409-07:00","url":"https://www.academia.edu/4173808/Extra_Solar_Planetary_Systems_A_Microcomputer_Simulation?f_ri=334552","dom_id":"work_4173808","summary":"\"\"Knowledge of the physical and chemical processes which occur within the circum-stellar nebula of a newly formed star is still uncertain and permits a number of distinct theories to account for the formation of planets. In order to gain a greater insight into the complexities of planetary formation, researchers have concentrated on 'realistic' simulations of clearly defined and limited aspects of the problem of the formation of the Solar System. Attempts to describe the nature of planetary systems of other stars have been left largely to popular speculation.\r\nThe microcomputer model presented here produces a wide range of data for possible planetary systems with primary stars in the mass range 0.6 - 1.3 M⊙. A synthesis of current theory, research and speculation, the purpose of this model is not to add to our understanding of the processes that form planets, but to give an integrated view of the possible nature of extra-solar planetary systems and to investigate the possibility of a systematic variation in planetary characteristics with primary mass. \"\"","downloadable_attachments":[{"id":31676329,"asset_id":4173808,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_38560094 coauthored" data-work_id="38560094" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/38560094/Evidence_of_Life_on_Mars">Evidence of Life on Mars</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Evidence is reviewed which supports the hypothesis that prokaryotes and eukaryotes may have colonized Mars. One source of Martian life, is Earth. A variety of species remain viable after long term exposure to the radiation intense... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_38560094" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Evidence is reviewed which supports the hypothesis that prokaryotes and eukaryotes may have colonized Mars. One source of Martian life, is Earth. A variety of species remain viable after long term exposure to the radiation intense environment of space, and may survive ejection from Earth following meteor strikes, ejection from the stratosphere and mesosphere via solar winds, and sterilization of Mars-bound spacecraft; whereas simulations studies have shown that prokaryotes, fungi and lichens survive in simulated Martian environments-findings which support the hypothesis life may have been repeatedly transferred from Earth to Mars. Four independent investigators have reported what appears to be fungi and lichens on the Martian surface, whereas a fifth investigator reported what may be cyanobacteria. In another study, a statistically significant majority of 70 experts, after examining Martian specimens photographed by NASA, identified and agreed fungi, basidiomycota ("puffballs"), and lichens may have colonized Mars. Fifteen specimens resembling and identified as "puffballs" were photographed emerging from the ground over a three day period. It is possible these latter specimens are hematite and what appears to be "growth" is due to a strong wind which uncovered these specimens-an explanation which cannot account for before and after photos of what appears to be masses of fungi growing atop and within the Mars rovers. Terrestrial hematite is in part fashioned and cemented together by prokaryotes and fungi, and thus Martian hematite may also be evidence of biology. Three independent research teams have identified sediments on Mars resembling stromatolites and outcroppings having micro meso and macro characteristics typical of terrestrial microbialites constructed by cyanobacteria. Quantitative morphological analysis determined these latter specimens are statistically and physically similar to terrestrial stromatolites. Reports of water, biological residue discovered in Martian meteor ALH84001, the seasonal waning and waxing of atmospheric and ground level Martian methane which on Earth is 90% due to biology and plant growth and decay, and results from the 1976 Mars Viking Labeled Release Experiments indicating biological activity, also support the hypothesis that Mars was, and is, a living planet. Nevertheless, much of the evidence remains circumstantial and unverified, and the possibility of life on Mars remains an open question.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/38560094" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="a17004927ef928a9700e53b5c1604a7a" rel="nofollow" data-download="{"attachment_id":58632178,"asset_id":38560094,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/58632178/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="64519228" href="https://independent.academia.edu/RGabrielJoseph">Rhawn Gabriel Joseph</a><script data-card-contents-for-user="64519228" type="text/json">{"id":64519228,"first_name":"Rhawn Gabriel","last_name":"Joseph","domain_name":"independent","page_name":"RGabrielJoseph","display_name":"Rhawn Gabriel Joseph","profile_url":"https://independent.academia.edu/RGabrielJoseph?f_ri=334552","photo":"/images/s65_no_pic.png"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-38560094">+1</span><div class="hidden js-additional-users-38560094"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://unisi.academia.edu/GiorgioBianciardi">Giorgio Bianciardi</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-38560094'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-38560094').html(); } } new HoverPopover(popoverSettings); })();</script></li><li class="js-paper-rank-work_38560094 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="38560094"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 38560094, container: ".js-paper-rank-work_38560094", }); });</script></li><li class="js-percentile-work_38560094 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 38560094; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_38560094"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_38560094 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="38560094"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 38560094; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=38560094]").text(description); $(".js-view-count-work_38560094").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_38560094").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="38560094"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">15</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="9752" href="https://www.academia.edu/Documents/in/Cyanobacteria">Cyanobacteria</a>, <script data-card-contents-for-ri="9752" type="text/json">{"id":9752,"name":"Cyanobacteria","url":"https://www.academia.edu/Documents/in/Cyanobacteria?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="13320" href="https://www.academia.edu/Documents/in/Mars">Mars</a>, <script data-card-contents-for-ri="13320" type="text/json">{"id":13320,"name":"Mars","url":"https://www.academia.edu/Documents/in/Mars?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="17272" href="https://www.academia.edu/Documents/in/Fungi">Fungi</a><script data-card-contents-for-ri="17272" type="text/json">{"id":17272,"name":"Fungi","url":"https://www.academia.edu/Documents/in/Fungi?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=38560094]'), work: {"id":38560094,"title":"Evidence of Life on Mars","created_at":"2019-03-15T16:24:03.132-07:00","url":"https://www.academia.edu/38560094/Evidence_of_Life_on_Mars?f_ri=334552","dom_id":"work_38560094","summary":"Evidence is reviewed which supports the hypothesis that prokaryotes and eukaryotes may have colonized Mars. One source of Martian life, is Earth. A variety of species remain viable after long term exposure to the radiation intense environment of space, and may survive ejection from Earth following meteor strikes, ejection from the stratosphere and mesosphere via solar winds, and sterilization of Mars-bound spacecraft; whereas simulations studies have shown that prokaryotes, fungi and lichens survive in simulated Martian environments-findings which support the hypothesis life may have been repeatedly transferred from Earth to Mars. Four independent investigators have reported what appears to be fungi and lichens on the Martian surface, whereas a fifth investigator reported what may be cyanobacteria. In another study, a statistically significant majority of 70 experts, after examining Martian specimens photographed by NASA, identified and agreed fungi, basidiomycota (\"puffballs\"), and lichens may have colonized Mars. Fifteen specimens resembling and identified as \"puffballs\" were photographed emerging from the ground over a three day period. It is possible these latter specimens are hematite and what appears to be \"growth\" is due to a strong wind which uncovered these specimens-an explanation which cannot account for before and after photos of what appears to be masses of fungi growing atop and within the Mars rovers. Terrestrial hematite is in part fashioned and cemented together by prokaryotes and fungi, and thus Martian hematite may also be evidence of biology. Three independent research teams have identified sediments on Mars resembling stromatolites and outcroppings having micro meso and macro characteristics typical of terrestrial microbialites constructed by cyanobacteria. Quantitative morphological analysis determined these latter specimens are statistically and physically similar to terrestrial stromatolites. Reports of water, biological residue discovered in Martian meteor ALH84001, the seasonal waning and waxing of atmospheric and ground level Martian methane which on Earth is 90% due to biology and plant growth and decay, and results from the 1976 Mars Viking Labeled Release Experiments indicating biological activity, also support the hypothesis that Mars was, and is, a living planet. Nevertheless, much of the evidence remains circumstantial and unverified, and the possibility of life on Mars remains an open question.","downloadable_attachments":[{"id":58632178,"asset_id":38560094,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":64519228,"first_name":"Rhawn Gabriel","last_name":"Joseph","domain_name":"independent","page_name":"RGabrielJoseph","display_name":"Rhawn Gabriel Joseph","profile_url":"https://independent.academia.edu/RGabrielJoseph?f_ri=334552","photo":"/images/s65_no_pic.png"},{"id":36668079,"first_name":"Giorgio","last_name":"Bianciardi","domain_name":"unisi","page_name":"GiorgioBianciardi","display_name":"Giorgio Bianciardi","profile_url":"https://unisi.academia.edu/GiorgioBianciardi?f_ri=334552","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":9752,"name":"Cyanobacteria","url":"https://www.academia.edu/Documents/in/Cyanobacteria?f_ri=334552","nofollow":false},{"id":13320,"name":"Mars","url":"https://www.academia.edu/Documents/in/Mars?f_ri=334552","nofollow":false},{"id":17272,"name":"Fungi","url":"https://www.academia.edu/Documents/in/Fungi?f_ri=334552","nofollow":false},{"id":17575,"name":"Algae","url":"https://www.academia.edu/Documents/in/Algae?f_ri=334552"},{"id":18862,"name":"Extremophiles","url":"https://www.academia.edu/Documents/in/Extremophiles?f_ri=334552"},{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552"},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552"},{"id":61024,"name":"Nasa","url":"https://www.academia.edu/Documents/in/Nasa?f_ri=334552"},{"id":75807,"name":"Astrobiology~(a) How did life begin on earth? (b) Is there any life outside the solar system?","url":"https://www.academia.edu/Documents/in/Astrobiology_a_How_did_life_begin_on_earth_b_Is_there_any_life_outside_the_solar_system?f_ri=334552"},{"id":149132,"name":"Lichens","url":"https://www.academia.edu/Documents/in/Lichens?f_ri=334552"},{"id":161213,"name":"Panspermia","url":"https://www.academia.edu/Documents/in/Panspermia?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":531200,"name":"Extraterrestrial Life","url":"https://www.academia.edu/Documents/in/Extraterrestrial_Life?f_ri=334552"},{"id":1361803,"name":"Puffballs","url":"https://www.academia.edu/Documents/in/Puffballs?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_44703950" data-work_id="44703950" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/44703950/Detection_of_pre_industrial_societies_on_exoplanets">Detection of pre-industrial societies on exoplanets</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Currently reading: Abstract Get access Share Cite Rights & Permissions [Opens in a new window] Abstract Approximately 22% of sun-like stars have Earth-like exoplanets. Advanced civilizations may exist on these, and significant effort... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_44703950" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Currently reading:<br />Abstract<br />Get access<br /><br />Share<br /><br />Cite<br />Rights & Permissions<br />[Opens in a new window]<br />Abstract<br />Approximately 22% of sun-like stars have Earth-like exoplanets. Advanced civilizations may exist on these, and significant effort has been expended on the theoretical analysis of planetary systems, and accompanying practical detection instruments.<br /><br />The longevity of technological civilizations is unknown, as is the probability of less advanced societies becoming technological. Accordingly, searching for pre-industrial extra-terrestrial societies may be more productive.<br /><br />Using the earth as a model, a consideration of possible detectible proxies suggests that observation of seasonal agriculture may be possible in the near future – particularly in ideal circumstances, for which quantitative analysis is provided. More speculatively, other detectible processes may include: species introduction; climate change; large urban fires and land-use or aquatic changes.<br /><br />Primitive societies may be both aware that their activities may be observed from other planets, and may deliberately adjust these activities to aid or conceal detection.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/44703950" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="f90b13cb25132d4ce9656c2f5fcd3050" rel="nofollow" data-download="{"attachment_id":65181797,"asset_id":44703950,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/65181797/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="16446192" href="https://ucl.academia.edu/AndrewLockley">Andrew Lockley</a><script data-card-contents-for-user="16446192" type="text/json">{"id":16446192,"first_name":"Andrew","last_name":"Lockley","domain_name":"ucl","page_name":"AndrewLockley","display_name":"Andrew Lockley","profile_url":"https://ucl.academia.edu/AndrewLockley?f_ri=334552","photo":"https://0.academia-photos.com/16446192/4478962/35481100/s65_andrew.lockley.jpg"}</script></span></span></li><li class="js-paper-rank-work_44703950 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="44703950"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 44703950, container: ".js-paper-rank-work_44703950", }); 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$(".js-view-count[data-work-id=44703950]").text(description); $(".js-view-count-work_44703950").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_44703950").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="44703950"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">3</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=44703950]'), work: {"id":44703950,"title":"Detection of pre-industrial societies on exoplanets","created_at":"2020-12-14T12:32:38.800-08:00","url":"https://www.academia.edu/44703950/Detection_of_pre_industrial_societies_on_exoplanets?f_ri=334552","dom_id":"work_44703950","summary":"Currently reading:\nAbstract\nGet access\n\nShare\n\nCite\nRights \u0026 Permissions\n[Opens in a new window]\nAbstract\nApproximately 22% of sun-like stars have Earth-like exoplanets. Advanced civilizations may exist on these, and significant effort has been expended on the theoretical analysis of planetary systems, and accompanying practical detection instruments.\n\nThe longevity of technological civilizations is unknown, as is the probability of less advanced societies becoming technological. Accordingly, searching for pre-industrial extra-terrestrial societies may be more productive.\n\nUsing the earth as a model, a consideration of possible detectible proxies suggests that observation of seasonal agriculture may be possible in the near future – particularly in ideal circumstances, for which quantitative analysis is provided. More speculatively, other detectible processes may include: species introduction; climate change; large urban fires and land-use or aquatic changes.\n\nPrimitive societies may be both aware that their activities may be observed from other planets, and may deliberately adjust these activities to aid or conceal detection.","downloadable_attachments":[{"id":65181797,"asset_id":44703950,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":16446192,"first_name":"Andrew","last_name":"Lockley","domain_name":"ucl","page_name":"AndrewLockley","display_name":"Andrew Lockley","profile_url":"https://ucl.academia.edu/AndrewLockley?f_ri=334552","photo":"https://0.academia-photos.com/16446192/4478962/35481100/s65_andrew.lockley.jpg"}],"research_interests":[{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_49090548 coauthored" data-work_id="49090548" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/49090548/The_Exploration_of_Habitable_Exoplanets_using_Data_Mining_Algorithms_and_Data_Manipulation">The Exploration of Habitable Exoplanets using Data Mining Algorithms and Data Manipulation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The NASA Exoplanet Archive is a dataset that is an extraction from the total sets of data from the Keck, Kepler, TESS, and Gaia observations, where observations show that the observed stellar objects have been determined to possess one or... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_49090548" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The NASA Exoplanet Archive is a dataset that is an extraction from the total sets of data from the Keck, Kepler, TESS, and Gaia observations, where observations show that the observed stellar objects have been determined to possess one or more planets. It is continually updated as more and more exoplanets, or planets outside our own solar system, are discovered and documented. Our first objective was to see how many of these entries were duplicates, which would bring the total number of entries we would work with from 29,283 to 4,259. In previous research, this dataset was filtered by determining which of these exoplanets are inside their Circumstellar Habitable-Zone (CHZ), commonly defined as the range of distance from a host star such that a planet may contain liquid water, a key requirement for life as we know it. However, this calculation was done only for exoplanets with M-type host stars. Over the course of our research, we were able to expand this calculation of the CHZ to exoplanets with host stars of all spectral types. We performed more in-depth investigation of planets with G, K, and M types stars by comparing them to planets in the Planetary Habitable Labratory (PHL) exoplanet dataset to see how many similarities there are. The PHL catalog used its own set of criteria to define those planets in it as habitable. Using this method, we determined that there were 3 exoplanets with M-type host stars, 0 exoplanets with a G-type host star, and 1 exoplanet with a Ktype host star.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/49090548" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="69197049879a1b202f85ccad9d3ba3fc" rel="nofollow" data-download="{"attachment_id":67485832,"asset_id":49090548,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/67485832/download_file?st=MTczMjM5NTQ0MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="99622950" href="https://1js22j.academia.edu/RobertDowningII">Robert A Downing II</a><script data-card-contents-for-user="99622950" type="text/json">{"id":99622950,"first_name":"Robert","last_name":"Downing II","domain_name":"1js22j","page_name":"RobertDowningII","display_name":"Robert A Downing II","profile_url":"https://1js22j.academia.edu/RobertDowningII?f_ri=334552","photo":"https://0.academia-photos.com/99622950/22331880/27735429/s65_robert.downing.jpg"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-49090548">+7</span><div class="hidden js-additional-users-49090548"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/HrithikPai">Hrithik Pai</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/SrideepDornala">Srideep Dornala</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/AlyNathoo">Aly Nathoo</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/SarinaMayya">Sarina Mayya</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/OjaswUpadhyay">Ojasw Upadhyay</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/ShashankRajan1">Shashank Karthik Rajan</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/PrachiS21">Prachi S</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-49090548'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-49090548').html(); 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container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_49090548 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="49090548"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 49090548; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=49090548]").text(description); $(".js-view-count-work_49090548").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_49090548").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="49090548"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">4</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="2008" href="https://www.academia.edu/Documents/in/Machine_Learning">Machine Learning</a>, <script data-card-contents-for-ri="2008" type="text/json">{"id":2008,"name":"Machine Learning","url":"https://www.academia.edu/Documents/in/Machine_Learning?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a>, <script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=49090548]'), work: {"id":49090548,"title":"The Exploration of Habitable Exoplanets using Data Mining Algorithms and Data Manipulation","created_at":"2021-06-01T13:07:04.605-07:00","url":"https://www.academia.edu/49090548/The_Exploration_of_Habitable_Exoplanets_using_Data_Mining_Algorithms_and_Data_Manipulation?f_ri=334552","dom_id":"work_49090548","summary":"The NASA Exoplanet Archive is a dataset that is an extraction from the total sets of data from the Keck, Kepler, TESS, and Gaia observations, where observations show that the observed stellar objects have been determined to possess one or more planets. It is continually updated as more and more exoplanets, or planets outside our own solar system, are discovered and documented. Our first objective was to see how many of these entries were duplicates, which would bring the total number of entries we would work with from 29,283 to 4,259. In previous research, this dataset was filtered by determining which of these exoplanets are inside their Circumstellar Habitable-Zone (CHZ), commonly defined as the range of distance from a host star such that a planet may contain liquid water, a key requirement for life as we know it. However, this calculation was done only for exoplanets with M-type host stars. Over the course of our research, we were able to expand this calculation of the CHZ to exoplanets with host stars of all spectral types. We performed more in-depth investigation of planets with G, K, and M types stars by comparing them to planets in the Planetary Habitable Labratory (PHL) exoplanet dataset to see how many similarities there are. The PHL catalog used its own set of criteria to define those planets in it as habitable. Using this method, we determined that there were 3 exoplanets with M-type host stars, 0 exoplanets with a G-type host star, and 1 exoplanet with a Ktype host star.","downloadable_attachments":[{"id":67485832,"asset_id":49090548,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":99622950,"first_name":"Robert","last_name":"Downing II","domain_name":"1js22j","page_name":"RobertDowningII","display_name":"Robert A Downing II","profile_url":"https://1js22j.academia.edu/RobertDowningII?f_ri=334552","photo":"https://0.academia-photos.com/99622950/22331880/27735429/s65_robert.downing.jpg"},{"id":174030512,"first_name":"Hrithik","last_name":"Pai","domain_name":"independent","page_name":"HrithikPai","display_name":"Hrithik Pai","profile_url":"https://independent.academia.edu/HrithikPai?f_ri=334552","photo":"https://0.academia-photos.com/174030512/48523259/38495965/s65_hrithik.pai.jpg"},{"id":195243577,"first_name":"Srideep","last_name":"Dornala","domain_name":"independent","page_name":"SrideepDornala","display_name":"Srideep Dornala","profile_url":"https://independent.academia.edu/SrideepDornala?f_ri=334552","photo":"https://0.academia-photos.com/195243577/57642320/45863058/s65_srideep.dornala.png"},{"id":195162400,"first_name":"Aly","last_name":"Nathoo","domain_name":"independent","page_name":"AlyNathoo","display_name":"Aly Nathoo","profile_url":"https://independent.academia.edu/AlyNathoo?f_ri=334552","photo":"https://0.academia-photos.com/195162400/61876400/133105302/s65_aly.nathoo.jpeg"},{"id":166882432,"first_name":"Sarina","last_name":"Mayya","domain_name":"independent","page_name":"SarinaMayya","display_name":"Sarina Mayya","profile_url":"https://independent.academia.edu/SarinaMayya?f_ri=334552","photo":"/images/s65_no_pic.png"},{"id":164560070,"first_name":"Ojasw","last_name":"Upadhyay","domain_name":"independent","page_name":"OjaswUpadhyay","display_name":"Ojasw Upadhyay","profile_url":"https://independent.academia.edu/OjaswUpadhyay?f_ri=334552","photo":"https://gravatar.com/avatar/eee25e66413c4328e3160ce68ef738db?s=65"},{"id":196409388,"first_name":"Shashank Karthik","last_name":"Rajan","domain_name":"independent","page_name":"ShashankRajan1","display_name":"Shashank Karthik Rajan","profile_url":"https://independent.academia.edu/ShashankRajan1?f_ri=334552","photo":"https://0.academia-photos.com/196409388/58670993/46905524/s65_shashank.rajan.jpeg"},{"id":236407280,"first_name":"Prachi","last_name":"S","domain_name":"independent","page_name":"PrachiS21","display_name":"Prachi S","profile_url":"https://independent.academia.edu/PrachiS21?f_ri=334552","photo":"https://0.academia-photos.com/236407280/92074723/80902444/s65_prachi.s.png"}],"research_interests":[{"id":2008,"name":"Machine Learning","url":"https://www.academia.edu/Documents/in/Machine_Learning?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_69899409" data-work_id="69899409" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/69899409/The_Search_for_Extraterrestrial_Life_in_the_Universe">The Search for Extraterrestrial Life in the Universe</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Remember that famous “I Want to Believe” poster of an Alien Spacecraft in Fox Mulder’s office in the famed TV series “The X Files”? The classic question of “Are we alone in this universe” has fascinated us for generations. According to... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_69899409" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Remember that famous “I Want to Believe” poster of an Alien Spacecraft in Fox Mulder’s office in the famed TV series “The X Files”? The classic question of “Are we alone in this universe” has fascinated us for generations. According to the Hubble Space Telescope’s findings, there are at least 125 billion+ galaxies in the universe, and at least 10% of all sun-like stars have a system of planets, and there are billions of stars with planets orbiting around them in the universe. And, even a billionth of these stars have planets that support life, then, there are around 6.25 billion life-supporting solar systems in this universe alone! <br /> <br />Let’s understand the logic behind the possibility of extra-terrestrial life forms in this following way: everything that we know of this universe, are known to exist in numbering more than one, like for example, we know for a fact that, there are more than one stars, (more than one) galaxies, (more than one) black holes, (more than one) nebula, (more than one) solar systems, (more than one) planets, (more than one) comets, asteroids, quasars, pulsars, and so on. Therefore, if everything in this universe exist in numbering more than one, then, why there should be only one planet in the universe like that of earth, a planet that is perfect for the sustenance of life? If the very natural order that built and sustained this universe, where all that exist (and ever existed), thrive in billions and billions in number, then shouldn’t there be more than one planet like that of earth in this universe, the very cosmos where everything is in their millions to billions to even more? <br /> <br />Truth is, concerns over extraterrestrial life forms are as much spiritual as they are scientific. And, this book aims to prove that, the possibility of extra-terrestrial life is very much real and WE ARE DEFINITELY, ABSOLUTELY, AND CERTAINLY NOT ALONE IN THIS UNIVERSE!!!</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/69899409" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="735e836c3275004fcdadb19aa4477a9e" rel="nofollow" data-download="{"attachment_id":85474147,"asset_id":69899409,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/85474147/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="66456548" href="https://independent.academia.edu/ObaidurRahman26">Obaidur Rahman</a><script data-card-contents-for-user="66456548" type="text/json">{"id":66456548,"first_name":"Obaidur","last_name":"Rahman","domain_name":"independent","page_name":"ObaidurRahman26","display_name":"Obaidur Rahman","profile_url":"https://independent.academia.edu/ObaidurRahman26?f_ri=334552","photo":"https://0.academia-photos.com/66456548/17627408/67725784/s65_obaidur.rahman.jpg"}</script></span></span></li><li class="js-paper-rank-work_69899409 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="69899409"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 69899409, container: ".js-paper-rank-work_69899409", }); 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The classic question of “Are we alone in this universe” has fascinated us for generations. According to the Hubble Space Telescope’s findings, there are at least 125 billion+ galaxies in the universe, and at least 10% of all sun-like stars have a system of planets, and there are billions of stars with planets orbiting around them in the universe. And, even a billionth of these stars have planets that support life, then, there are around 6.25 billion life-supporting solar systems in this universe alone!\r\n\r\nLet’s understand the logic behind the possibility of extra-terrestrial life forms in this following way: everything that we know of this universe, are known to exist in numbering more than one, like for example, we know for a fact that, there are more than one stars, (more than one) galaxies, (more than one) black holes, (more than one) nebula, (more than one) solar systems, (more than one) planets, (more than one) comets, asteroids, quasars, pulsars, and so on. Therefore, if everything in this universe exist in numbering more than one, then, why there should be only one planet in the universe like that of earth, a planet that is perfect for the sustenance of life? If the very natural order that built and sustained this universe, where all that exist (and ever existed), thrive in billions and billions in number, then shouldn’t there be more than one planet like that of earth in this universe, the very cosmos where everything is in their millions to billions to even more?\r\n\r\nTruth is, concerns over extraterrestrial life forms are as much spiritual as they are scientific. And, this book aims to prove that, the possibility of extra-terrestrial life is very much real and WE ARE DEFINITELY, ABSOLUTELY, AND CERTAINLY NOT ALONE IN THIS UNIVERSE!!!","downloadable_attachments":[{"id":85474147,"asset_id":69899409,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":66456548,"first_name":"Obaidur","last_name":"Rahman","domain_name":"independent","page_name":"ObaidurRahman26","display_name":"Obaidur Rahman","profile_url":"https://independent.academia.edu/ObaidurRahman26?f_ri=334552","photo":"https://0.academia-photos.com/66456548/17627408/67725784/s65_obaidur.rahman.jpg"}],"research_interests":[{"id":400,"name":"Earth Sciences","url":"https://www.academia.edu/Documents/in/Earth_Sciences?f_ri=334552","nofollow":false},{"id":2417,"name":"Planetary Science","url":"https://www.academia.edu/Documents/in/Planetary_Science?f_ri=334552","nofollow":false},{"id":6756,"name":"Conspiracy Theories","url":"https://www.academia.edu/Documents/in/Conspiracy_Theories?f_ri=334552","nofollow":false},{"id":7091,"name":"History of Space Travel","url":"https://www.academia.edu/Documents/in/History_of_Space_Travel?f_ri=334552","nofollow":false},{"id":9883,"name":"Human Spaceflight","url":"https://www.academia.edu/Documents/in/Human_Spaceflight?f_ri=334552"},{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552"},{"id":37604,"name":"UFOlogy","url":"https://www.academia.edu/Documents/in/UFOlogy?f_ri=334552"},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552"},{"id":61024,"name":"Nasa","url":"https://www.academia.edu/Documents/in/Nasa?f_ri=334552"},{"id":77513,"name":"Origin of Universe","url":"https://www.academia.edu/Documents/in/Origin_of_Universe?f_ri=334552"},{"id":93741,"name":"Cosmos","url":"https://www.academia.edu/Documents/in/Cosmos?f_ri=334552"},{"id":105017,"name":"Ancient Aliens","url":"https://www.academia.edu/Documents/in/Ancient_Aliens?f_ri=334552"},{"id":138103,"name":"Aliens","url":"https://www.academia.edu/Documents/in/Aliens?f_ri=334552"},{"id":259533,"name":"Extra-Terrestrial life","url":"https://www.academia.edu/Documents/in/Extra-Terrestrial_life?f_ri=334552"},{"id":309434,"name":"Solar System","url":"https://www.academia.edu/Documents/in/Solar_System?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":675517,"name":"Physics and Astronomy","url":"https://www.academia.edu/Documents/in/Physics_and_Astronomy?f_ri=334552"},{"id":974606,"name":"Astrobiology/Exobiology","url":"https://www.academia.edu/Documents/in/Astrobiology_Exobiology?f_ri=334552"},{"id":1222265,"name":"XX Century ET/Alien/UFO \"contactee\" discourses","url":"https://www.academia.edu/Documents/in/XX_Century_ET_Alien_UFO_contactee_discourses?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_40322118" data-work_id="40322118" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/40322118/Searching_for_New_Earth">Searching for New Earth</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The discovery of exoplanets has intensified interest in the search for extraterrestrial life, especially for planets orbiting the sun like stars in habitable zone. The study of planetary habitability also considers a wide range of other... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_40322118" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The discovery of exoplanets has intensified interest in the search for extraterrestrial life, especially for planets orbiting the sun like stars in habitable zone. The study of planetary habitability also considers a wide range of other factors in determining the suitability of a planet for hosting life. This study aims to determine to explore the variety exoplanets like giant planets, terrestrial planets, habitable planets, and earth like planets. The method for searching that planets are using five different methods, like radial velocity method, transit method, gravitational micro-lensing, astrometry, and direct imaging. From the study process obtained that there are 1.271 giant planets, 211 terrestrial planets, 291 habitable planets, and 2 earth like planets.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/40322118" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="d05c6034b5a9adacdd44edcc652217af" rel="nofollow" data-download="{"attachment_id":60564624,"asset_id":40322118,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/60564624/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="9997491" href="https://usu-id.academia.edu/BerthiannaNurcresia">Berthianna Nurcresia</a><script data-card-contents-for-user="9997491" type="text/json">{"id":9997491,"first_name":"Berthianna","last_name":"Nurcresia","domain_name":"usu-id","page_name":"BerthiannaNurcresia","display_name":"Berthianna Nurcresia","profile_url":"https://usu-id.academia.edu/BerthiannaNurcresia?f_ri=334552","photo":"https://0.academia-photos.com/9997491/3741791/38778696/s65_berthianna.nurcresia.jpg"}</script></span></span></li><li class="js-paper-rank-work_40322118 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="40322118"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 40322118, container: ".js-paper-rank-work_40322118", }); 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The study of planetary habitability also considers a wide range of other factors in determining the suitability of a planet for hosting life. This study aims to determine to explore the variety exoplanets like giant planets, terrestrial planets, habitable planets, and earth like planets. The method for searching that planets are using five different methods, like radial velocity method, transit method, gravitational micro-lensing, astrometry, and direct imaging. From the study process obtained that there are 1.271 giant planets, 211 terrestrial planets, 291 habitable planets, and 2 earth like planets.","downloadable_attachments":[{"id":60564624,"asset_id":40322118,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":9997491,"first_name":"Berthianna","last_name":"Nurcresia","domain_name":"usu-id","page_name":"BerthiannaNurcresia","display_name":"Berthianna Nurcresia","profile_url":"https://usu-id.academia.edu/BerthiannaNurcresia?f_ri=334552","photo":"https://0.academia-photos.com/9997491/3741791/38778696/s65_berthianna.nurcresia.jpg"}],"research_interests":[{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4156589" data-work_id="4156589" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4156589/A_Planet_Dwellers_Dreams">A Planet Dweller's Dreams</a></div></div><div class="u-pb4x u-mt3x"></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4156589" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="111ba2fecfd4d72fc1689de3a181867c" rel="nofollow" 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type="text/json">{"id":278703,"name":"Terraforming","url":"https://www.academia.edu/Documents/in/Terraforming?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4156589]'), work: {"id":4156589,"title":"A Planet Dweller's 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u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="26474960" href="https://independent.academia.edu/MillenniumTwain">Millennium Twain</a><script data-card-contents-for-user="26474960" type="text/json">{"id":26474960,"first_name":"Millennium","last_name":"Twain","domain_name":"independent","page_name":"MillenniumTwain","display_name":"Millennium Twain","profile_url":"https://independent.academia.edu/MillenniumTwain?f_ri=334552","photo":"https://0.academia-photos.com/26474960/7346872/8261291/s65_millennium.twain.jpg"}</script></span></span></li><li class="js-paper-rank-work_11143555 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="11143555"><i class="u-m1x fa fa-bar-chart"></i><strong 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href="https://www.academia.edu/Documents/in/Observational_Astronomy">Observational Astronomy</a><script data-card-contents-for-ri="702" type="text/json">{"id":702,"name":"Observational Astronomy","url":"https://www.academia.edu/Documents/in/Observational_Astronomy?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=11143555]'), work: {"id":11143555,"title":"Sirius Shift, Sirius (Parallax) Disclosure!","created_at":"2015-02-27T07:13:09.685-08:00","url":"https://www.academia.edu/11143555/Sirius_Shift_Sirius_Parallax_Disclosure_?f_ri=334552","dom_id":"work_11143555","summary":"Introduction to Stellar Parallax and Stellar Distance Corrections from Military to Public Sector 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Astronomy","url":"https://www.academia.edu/Documents/in/Observational_Astronomy?f_ri=334552","nofollow":false},{"id":710,"name":"Stellar Astrophysics","url":"https://www.academia.edu/Documents/in/Stellar_Astrophysics?f_ri=334552"},{"id":3641,"name":"Aeronautical Engineering","url":"https://www.academia.edu/Documents/in/Aeronautical_Engineering?f_ri=334552"},{"id":4112,"name":"Theoretical astrophysics","url":"https://www.academia.edu/Documents/in/Theoretical_astrophysics?f_ri=334552"},{"id":4535,"name":"Space astronomy","url":"https://www.academia.edu/Documents/in/Space_astronomy?f_ri=334552"},{"id":9010,"name":"Astronautics","url":"https://www.academia.edu/Documents/in/Astronautics?f_ri=334552"},{"id":10088,"name":"History of Astronomy","url":"https://www.academia.edu/Documents/in/History_of_Astronomy?f_ri=334552"},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552"},{"id":12105,"name":"Aeronautics and Aerospace Operations","url":"https://www.academia.edu/Documents/in/Aeronautics_and_Aerospace_Operations?f_ri=334552"},{"id":14668,"name":"Aerospace","url":"https://www.academia.edu/Documents/in/Aerospace?f_ri=334552"},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552"},{"id":36190,"name":"Cultural Astronomy","url":"https://www.academia.edu/Documents/in/Cultural_Astronomy?f_ri=334552"},{"id":39286,"name":"Exoplanet detection","url":"https://www.academia.edu/Documents/in/Exoplanet_detection?f_ri=334552"},{"id":39288,"name":"Astrometry","url":"https://www.academia.edu/Documents/in/Astrometry?f_ri=334552"},{"id":41126,"name":"Ancient Astronomy","url":"https://www.academia.edu/Documents/in/Ancient_Astronomy?f_ri=334552"},{"id":41236,"name":"Extrasolar 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searches","url":"https://www.academia.edu/Documents/in/Extrasolar_planetary_searches?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":387387,"name":"VLBI","url":"https://www.academia.edu/Documents/in/VLBI?f_ri=334552"},{"id":434587,"name":"Space Exploration Direct /Indirect Detailed Imaging Exoplanets","url":"https://www.academia.edu/Documents/in/Space_Exploration_Direct_Indirect_Detailed_Imaging_Exoplanets?f_ri=334552"},{"id":497139,"name":"Extrasolar Planetary Systems","url":"https://www.academia.edu/Documents/in/Extrasolar_Planetary_Systems?f_ri=334552"},{"id":675517,"name":"Physics and Astronomy","url":"https://www.academia.edu/Documents/in/Physics_and_Astronomy?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4156845" data-work_id="4156845" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4156845/Terrestrial_Planet_Formation_in_Exoplanetary_Systems">Terrestrial Planet Formation in Exoplanetary Systems</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Many giant exoplanets are thought to have formed in the outer regions of a protoplanetary disk, and to have then migrated close to the central star. Hence, it is uncertain whether terrestrial planets can grow and be retained in these... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4156845" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Many giant exoplanets are thought to have formed in the outer regions of a protoplanetary <br />disk, and to have then migrated close to the central star. Hence, it is uncertain <br />whether terrestrial planets can grow and be retained in these `hot-Jupiter' systems. <br />Previous speculations, based on the assumption that migrating giant planets will clear <br />planet-forming material from their swept zone, have concluded that such systems <br />should lack terrestrial planets. <br />This thesis presents a succession of four planet formation models, of increasing <br />sophistication, aimed at examining how an inner system of solid bodies, undergoing <br />terrestrial planet formation, evolves under the inuence of a giant planet undergoing <br />inward type II migration. Protoplanetary growth is handled by an N+N'-body code, <br />capable of simulating the accretion of a two-phase protoplanetplanetesimal population, <br />and tracking their volatiles content. Gas dynamics and related dissipative processes <br />are calculated with a linked viscous gas disk algorithm capable of simulating: <br />gas accretion onto the central star and photoevaporation; type II migration of the giant <br />planet; type I migration of protoplanets; and the effect of gas drag on planetesimals. <br />In all simulations, a large fraction of the inner system material survives the passage <br />of the giant, either by accreting into massive planets shepherded inward of the <br />giant (reminiscent of the short-period `hot-Earths' discovered recently), or by being <br />scattered into external orbits. Typically, sufcient mass is scattered outward to provide <br />for the eventual accretion of a set of terrestrial planets in external orbits. <br />The results of this thesis lead to the prediction that hot-Jupiter systems are likely <br />to harbor water-rich terrestrial planets in their habitable zones and hot-Earths may <br />also be present. These planets may be detected by future planet search missions.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4156845" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="9a785e62d20cae6e84ea2fd4fbc3b63a" rel="nofollow" data-download="{"attachment_id":31663296,"asset_id":4156845,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31663296/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4156845 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4156845"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4156845, container: ".js-paper-rank-work_4156845", }); });</script></li><li class="js-percentile-work_4156845 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4156845; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4156845"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4156845 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4156845"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4156845; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4156845]").text(description); $(".js-view-count-work_4156845").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4156845").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4156845"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">9</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="2417" href="https://www.academia.edu/Documents/in/Planetary_Science">Planetary Science</a>, <script data-card-contents-for-ri="2417" type="text/json">{"id":2417,"name":"Planetary Science","url":"https://www.academia.edu/Documents/in/Planetary_Science?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a><script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4156845]'), work: {"id":4156845,"title":"Terrestrial Planet Formation in Exoplanetary Systems","created_at":"2013-08-01T19:18:33.258-07:00","url":"https://www.academia.edu/4156845/Terrestrial_Planet_Formation_in_Exoplanetary_Systems?f_ri=334552","dom_id":"work_4156845","summary":"Many giant exoplanets are thought to have formed in the outer regions of a protoplanetary\r\ndisk, and to have then migrated close to the central star. Hence, it is uncertain\r\nwhether terrestrial planets can grow and be retained in these `hot-Jupiter' systems.\r\nPrevious speculations, based on the assumption that migrating giant planets will clear\r\nplanet-forming material from their swept zone, have concluded that such systems\r\nshould lack terrestrial planets.\r\nThis thesis presents a succession of four planet formation models, of increasing\r\nsophistication, aimed at examining how an inner system of solid bodies, undergoing\r\nterrestrial planet formation, evolves under the in\u0003uence of a giant planet undergoing\r\ninward type II migration. Protoplanetary growth is handled by an N+N'-body code,\r\ncapable of simulating the accretion of a two-phase protoplanetplanetesimal population,\r\nand tracking their volatiles content. Gas dynamics and related dissipative processes\r\nare calculated with a linked viscous gas disk algorithm capable of simulating:\r\ngas accretion onto the central star and photoevaporation; type II migration of the giant\r\nplanet; type I migration of protoplanets; and the effect of gas drag on planetesimals.\r\nIn all simulations, a large fraction of the inner system material survives the passage\r\nof the giant, either by accreting into massive planets shepherded inward of the\r\ngiant (reminiscent of the short-period `hot-Earths' discovered recently), or by being\r\nscattered into external orbits. Typically, suf\u0002cient mass is scattered outward to provide\r\nfor the eventual accretion of a set of terrestrial planets in external orbits.\r\nThe results of this thesis lead to the prediction that hot-Jupiter systems are likely\r\nto harbor water-rich terrestrial planets in their habitable zones and hot-Earths may\r\nalso be present. These planets may be detected by future planet search missions.","downloadable_attachments":[{"id":31663296,"asset_id":4156845,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":2417,"name":"Planetary Science","url":"https://www.academia.edu/Documents/in/Planetary_Science?f_ri=334552","nofollow":false},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552"},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_36288962" data-work_id="36288962" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/36288962/Mencari_Bumi_yang_Baru">Mencari Bumi yang Baru</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Penemuan planet ekstrasolar telah mengintensifkan ketertarikan khusus dalam pencarian kehidupan di luar bumi, termasuk bagi planet yang mengorbit bintang induknya yang seperti Matahari dalam zona layak huni. Sampai saat ini studi mengenai... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_36288962" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Penemuan planet ekstrasolar telah mengintensifkan ketertarikan khusus dalam pencarian kehidupan di luar bumi, termasuk bagi planet yang mengorbit bintang induknya yang seperti Matahari dalam zona layak huni. Sampai saat ini studi mengenai kelayakhunian planet juga mempertimbangkan berbagai faktor lain dalam menentukan kelayakan planet untuk menampung kehidupan. Kajian ini bertujuan untuk mempelajari keberagaman banyak planet – planet ekstrasolar yang berupa planet raksasa, planet terrestrial, planet layak huni, dan planet mirip Bumi. pendeteksian planet – planet tersebut menggunakan lima metode beragam, yaitu metode kecepatan radial, transit, astrometri, mikrolensa gravitasi, dan pencitraan langsung. Dari proses pengkajian, telah di dapatkan bahwa ada sekitar 1.271 planet raksasa, 211 planet terrestrial, 291 planet layak huni, dan 2 planet mirip Bumi.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/36288962" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="7b6a9db00f9052c966fadac5f67dc575" rel="nofollow" data-download="{"attachment_id":56194843,"asset_id":36288962,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/56194843/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="9997491" href="https://usu-id.academia.edu/BerthiannaNurcresia">Berthianna Nurcresia</a><script data-card-contents-for-user="9997491" type="text/json">{"id":9997491,"first_name":"Berthianna","last_name":"Nurcresia","domain_name":"usu-id","page_name":"BerthiannaNurcresia","display_name":"Berthianna Nurcresia","profile_url":"https://usu-id.academia.edu/BerthiannaNurcresia?f_ri=334552","photo":"https://0.academia-photos.com/9997491/3741791/38778696/s65_berthianna.nurcresia.jpg"}</script></span></span></li><li class="js-paper-rank-work_36288962 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="36288962"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 36288962, container: ".js-paper-rank-work_36288962", }); });</script></li><li class="js-percentile-work_36288962 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 36288962; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_36288962"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_36288962 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="36288962"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 36288962; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=36288962]").text(description); $(".js-view-count-work_36288962").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_36288962").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="36288962"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a>, <script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="47599" href="https://www.academia.edu/Documents/in/Astronomy">Astronomy</a>, <script data-card-contents-for-ri="47599" type="text/json">{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="287963" href="https://www.academia.edu/Documents/in/Astronomi">Astronomi</a><script data-card-contents-for-ri="287963" type="text/json">{"id":287963,"name":"Astronomi","url":"https://www.academia.edu/Documents/in/Astronomi?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=36288962]'), work: {"id":36288962,"title":"Mencari Bumi yang Baru","created_at":"2018-03-29T22:35:33.327-07:00","url":"https://www.academia.edu/36288962/Mencari_Bumi_yang_Baru?f_ri=334552","dom_id":"work_36288962","summary":"Penemuan planet ekstrasolar telah mengintensifkan ketertarikan khusus dalam pencarian kehidupan di luar bumi, termasuk bagi planet yang mengorbit bintang induknya yang seperti Matahari dalam zona layak huni. Sampai saat ini studi mengenai kelayakhunian planet juga mempertimbangkan berbagai faktor lain dalam menentukan kelayakan planet untuk menampung kehidupan. Kajian ini bertujuan untuk mempelajari keberagaman banyak planet – planet ekstrasolar yang berupa planet raksasa, planet terrestrial, planet layak huni, dan planet mirip Bumi. pendeteksian planet – planet tersebut menggunakan lima metode beragam, yaitu metode kecepatan radial, transit, astrometri, mikrolensa gravitasi, dan pencitraan langsung. Dari proses pengkajian, telah di dapatkan bahwa ada sekitar 1.271 planet raksasa, 211 planet terrestrial, 291 planet layak huni, dan 2 planet mirip Bumi.\r\n","downloadable_attachments":[{"id":56194843,"asset_id":36288962,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":9997491,"first_name":"Berthianna","last_name":"Nurcresia","domain_name":"usu-id","page_name":"BerthiannaNurcresia","display_name":"Berthianna Nurcresia","profile_url":"https://usu-id.academia.edu/BerthiannaNurcresia?f_ri=334552","photo":"https://0.academia-photos.com/9997491/3741791/38778696/s65_berthianna.nurcresia.jpg"}],"research_interests":[{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false},{"id":287963,"name":"Astronomi","url":"https://www.academia.edu/Documents/in/Astronomi?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":675513,"name":"Earth and Planetary Sciences","url":"https://www.academia.edu/Documents/in/Earth_and_Planetary_Sciences?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_34106283 coauthored" data-work_id="34106283" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/34106283/Indexing_of_exoplanets_in_search_for_potential_habitability_application_to_Mars_like_worlds">Indexing of exoplanets in search for potential habitability: application to Mars-like worlds</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Study of exoplanets is one of the main goals of present research in planetary sciences and astrobiology. Analysis of huge planetary data from space missions such as CoRoT and Kepler is directed ultimately at finding a planet similar to... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_34106283" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Study of exoplanets is one of the main goals of present research in planetary sciences and astrobiology. Analysis of huge planetary data from space missions such as CoRoT and Kepler is directed ultimately at finding a planet similar to Earth—the Earth's twin, and answering the question of potential exo-habitability. The Earth Similarity Index (ESI) is a first step in this quest, ranging from 1 (Earth) to 0 (totally dissimilar to Earth). It was defined for the four physical parameters of a planet: radius, density, escape velocity and surface temperature. The ESI is further subdivided into interior ESI (geometrical mean of radius and density) and surface ESI (geometrical mean of escape velocity and surface temperature). The challenge here is to determine which exoplanet parameter(s) is important in finding this similarity ; how exactly the individual parameters entering the interior ESI and surface ESI are contributing to the global ESI. Since the surface temperature entering surface ESI is a non-observable quantity, it is difficult to determine its value. Using the known data for the Solar System objects, we established the calibration relation between surface and equilibrium temperatures to devise an effective way to estimate the value of the surface temperature of exoplanets. ESI is a first step in determining potential exo-habitability that may not be very similar to a terrestrial life. A new approach , called Mars Similarity Index (MSI), is introduced to identify planets that may be habitable to the extreme forms of life. MSI is defined in the range between 1 (present Mars) and 0 (dissimilar to present Mars) and uses the same physical parameters as ESI. We are interested in Mars-like planets to search for planets that may host the extreme life forms, such as the ones living in extreme environments on Earth; for example, methane on Mars may be a product of the methane-specific extremophile life form metabolism.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/34106283" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="3d8445948ee8756792d3049e18f248a5" rel="nofollow" data-download="{"attachment_id":54037708,"asset_id":34106283,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/54037708/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="24421060" href="https://iiap.academia.edu/MSafonova">Margarita Safonova</a><script data-card-contents-for-user="24421060" type="text/json">{"id":24421060,"first_name":"Margarita","last_name":"Safonova","domain_name":"iiap","page_name":"MSafonova","display_name":"Margarita Safonova","profile_url":"https://iiap.academia.edu/MSafonova?f_ri=334552","photo":"https://0.academia-photos.com/24421060/6587903/19041767/s65_margarita.safonova.jpg"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-34106283">+2</span><div class="hidden js-additional-users-34106283"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://christuniversity.academia.edu/MadhuKashyapJagadeesh">Madhu Kashyap Jagadeesh</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://christuniversity.academia.edu/ShivappaGudennavar">Shivappa Gudennavar</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-34106283'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-34106283').html(); } } new HoverPopover(popoverSettings); })();</script></li><li class="js-paper-rank-work_34106283 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="34106283"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 34106283, container: ".js-paper-rank-work_34106283", }); });</script></li><li class="js-percentile-work_34106283 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 34106283; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_34106283"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_34106283 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="34106283"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 34106283; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=34106283]").text(description); $(".js-view-count-work_34106283").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_34106283").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="34106283"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">3</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="75807" href="https://www.academia.edu/Documents/in/Astrobiology_a_How_did_life_begin_on_earth_b_Is_there_any_life_outside_the_solar_system">Astrobiology~(a) How did life begin on earth? (b) Is there any life outside the solar system?</a>, <script data-card-contents-for-ri="75807" type="text/json">{"id":75807,"name":"Astrobiology~(a) How did life begin on earth? (b) Is there any life outside the solar system?","url":"https://www.academia.edu/Documents/in/Astrobiology_a_How_did_life_begin_on_earth_b_Is_there_any_life_outside_the_solar_system?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a>, <script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="406486" href="https://www.academia.edu/Documents/in/Habitability">Habitability</a><script data-card-contents-for-ri="406486" type="text/json">{"id":406486,"name":"Habitability","url":"https://www.academia.edu/Documents/in/Habitability?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=34106283]'), work: {"id":34106283,"title":"Indexing of exoplanets in search for potential habitability: application to Mars-like worlds","created_at":"2017-08-02T02:38:39.483-07:00","url":"https://www.academia.edu/34106283/Indexing_of_exoplanets_in_search_for_potential_habitability_application_to_Mars_like_worlds?f_ri=334552","dom_id":"work_34106283","summary":"Study of exoplanets is one of the main goals of present research in planetary sciences and astrobiology. Analysis of huge planetary data from space missions such as CoRoT and Kepler is directed ultimately at finding a planet similar to Earth—the Earth's twin, and answering the question of potential exo-habitability. The Earth Similarity Index (ESI) is a first step in this quest, ranging from 1 (Earth) to 0 (totally dissimilar to Earth). It was defined for the four physical parameters of a planet: radius, density, escape velocity and surface temperature. The ESI is further subdivided into interior ESI (geometrical mean of radius and density) and surface ESI (geometrical mean of escape velocity and surface temperature). The challenge here is to determine which exoplanet parameter(s) is important in finding this similarity ; how exactly the individual parameters entering the interior ESI and surface ESI are contributing to the global ESI. Since the surface temperature entering surface ESI is a non-observable quantity, it is difficult to determine its value. Using the known data for the Solar System objects, we established the calibration relation between surface and equilibrium temperatures to devise an effective way to estimate the value of the surface temperature of exoplanets. ESI is a first step in determining potential exo-habitability that may not be very similar to a terrestrial life. A new approach , called Mars Similarity Index (MSI), is introduced to identify planets that may be habitable to the extreme forms of life. MSI is defined in the range between 1 (present Mars) and 0 (dissimilar to present Mars) and uses the same physical parameters as ESI. We are interested in Mars-like planets to search for planets that may host the extreme life forms, such as the ones living in extreme environments on Earth; for example, methane on Mars may be a product of the methane-specific extremophile life form metabolism.","downloadable_attachments":[{"id":54037708,"asset_id":34106283,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":24421060,"first_name":"Margarita","last_name":"Safonova","domain_name":"iiap","page_name":"MSafonova","display_name":"Margarita Safonova","profile_url":"https://iiap.academia.edu/MSafonova?f_ri=334552","photo":"https://0.academia-photos.com/24421060/6587903/19041767/s65_margarita.safonova.jpg"},{"id":67117599,"first_name":"Madhu Kashyap","last_name":"Jagadeesh","domain_name":"christuniversity","page_name":"MadhuKashyapJagadeesh","display_name":"Madhu Kashyap Jagadeesh","profile_url":"https://christuniversity.academia.edu/MadhuKashyapJagadeesh?f_ri=334552","photo":"https://0.academia-photos.com/67117599/17464444/17544324/s65_madhu_kashyap.jagadeesh.jpg"},{"id":10568050,"first_name":"Shivappa","last_name":"Gudennavar","domain_name":"christuniversity","page_name":"ShivappaGudennavar","display_name":"Shivappa Gudennavar","profile_url":"https://christuniversity.academia.edu/ShivappaGudennavar?f_ri=334552","photo":"https://0.academia-photos.com/10568050/7421083/8341216/s65_shivappa.b..gudennavar.jpg"}],"research_interests":[{"id":75807,"name":"Astrobiology~(a) How did life begin on earth? (b) Is there any life outside the solar system?","url":"https://www.academia.edu/Documents/in/Astrobiology_a_How_did_life_begin_on_earth_b_Is_there_any_life_outside_the_solar_system?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":406486,"name":"Habitability","url":"https://www.academia.edu/Documents/in/Habitability?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_44357846" data-work_id="44357846" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/44357846/UV_habitable_zones_around_M_stars">UV habitable zones around M stars</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">During the last decade there was a change in paradigm, which led to consider that terrestrial-type planets within liquid-water habitable zones (LW-HZ) around M stars can also be suitable places for the emergence and evolution of life.... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_44357846" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">During the last decade there was a change in paradigm, which led to consider that terrestrial-type planets within liquid-water habitable zones (LW-HZ) around M stars can also be suitable places for the emergence and evolution of life. Since many dMe stars emit large amount of UV radiation during flares, in this work we analyze the UV constrains for living systems on Earth-like planets around dM stars. We apply our model of UV habitable zone (UV-HZ, Buccino et al. 2006) to the three planetary systems around dM stars (HIP 74995, HIP 109388 and HIP 113020) observed by IUE and to two M-flare stars (AD Leo and EV Lac). In particular, HIP 74995 hosts a terrestrial planet in the LW-HZ, which is the exoplanet that most resembles our own Earth. We show, in general, that during the quiescent state there would not be enough UV radiation within the LW-HZ to trigger the biogenic processes and that this energy could be provided by flares of moderate intensity, while strong flares do not necessarily rule-out the possibility of life-bearing planets.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/44357846" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="11d2da80abf3b8e832419a1b9da2b99c" rel="nofollow" data-download="{"attachment_id":64752961,"asset_id":44357846,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/64752961/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="31221696" href="https://ajitha.academia.edu/GuillermoLemarchand">Guillermo A . Lemarchand</a><script data-card-contents-for-user="31221696" type="text/json">{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}</script></span></span></li><li class="js-paper-rank-work_44357846 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="44357846"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 44357846, container: ".js-paper-rank-work_44357846", }); });</script></li><li class="js-percentile-work_44357846 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 44357846; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_44357846"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_44357846 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="44357846"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 44357846; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=44357846]").text(description); $(".js-view-count-work_44357846").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_44357846").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="44357846"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a>, <script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="47599" href="https://www.academia.edu/Documents/in/Astronomy">Astronomy</a>, <script data-card-contents-for-ri="47599" type="text/json">{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="49201" href="https://www.academia.edu/Documents/in/Life_in_the_Universe">Life in the Universe</a>, <script data-card-contents-for-ri="49201" type="text/json">{"id":49201,"name":"Life in the Universe","url":"https://www.academia.edu/Documents/in/Life_in_the_Universe?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="168481" href="https://www.academia.edu/Documents/in/UV_Vis_spectroscopy">UV/Vis spectroscopy</a><script data-card-contents-for-ri="168481" type="text/json">{"id":168481,"name":"UV/Vis spectroscopy","url":"https://www.academia.edu/Documents/in/UV_Vis_spectroscopy?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=44357846]'), work: {"id":44357846,"title":"UV habitable zones around M stars","created_at":"2020-10-23T10:49:16.546-07:00","url":"https://www.academia.edu/44357846/UV_habitable_zones_around_M_stars?f_ri=334552","dom_id":"work_44357846","summary":"During the last decade there was a change in paradigm, which led to consider that terrestrial-type planets within liquid-water habitable zones (LW-HZ) around M stars can also be suitable places for the emergence and evolution of life. Since many dMe stars emit large amount of UV radiation during flares, in this work we analyze the UV constrains for living systems on Earth-like planets around dM stars. We apply our model of UV habitable zone (UV-HZ, Buccino et al. 2006) to the three planetary systems around dM stars (HIP 74995, HIP 109388 and HIP 113020) observed by IUE and to two M-flare stars (AD Leo and EV Lac). In particular, HIP 74995 hosts a terrestrial planet in the LW-HZ, which is the exoplanet that most resembles our own Earth. We show, in general, that during the quiescent state there would not be enough UV radiation within the LW-HZ to trigger the biogenic processes and that this energy could be provided by flares of moderate intensity, while strong flares do not necessarily rule-out the possibility of life-bearing planets.","downloadable_attachments":[{"id":64752961,"asset_id":44357846,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}],"research_interests":[{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false},{"id":49201,"name":"Life in the Universe","url":"https://www.academia.edu/Documents/in/Life_in_the_Universe?f_ri=334552","nofollow":false},{"id":168481,"name":"UV/Vis spectroscopy","url":"https://www.academia.edu/Documents/in/UV_Vis_spectroscopy?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_35543978" data-work_id="35543978" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/35543978/Hubble_Revisited_on_NASAs_50th_Anniversary_First_Confirmation_Planet_Kepler_22b_An_Exoplanet_in_a_Habitable_Zone">Hubble Revisited on NASA's 50th Anniversary First Confirmation: Planet Kepler-22b An Exoplanet in a Habitable Zone</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">One of the earliest identifications of an Earth like extra solar planet was made by the Kepler space observatory in 2012. Designated Kepler 22b, the object was located about 400 light years away near a star slightly cooler and less bright... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_35543978" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">One of the earliest identifications of an Earth like extra solar planet was made by the Kepler space observatory in 2012. Designated Kepler 22b, the object was located about 400 light years away near a star slightly cooler and less bright than the sun.  The description of the discovery describes the Kepler telescope, the history of planetary transits, the transit of Venus earlier that year - and one of its original observations.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/35543978" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="759bdf54f7b2bd1ff7bd95529b23590f" rel="nofollow" data-download="{"attachment_id":55409486,"asset_id":35543978,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/55409486/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="73357516" href="https://independent.academia.edu/kellywes">wes kelly</a><script data-card-contents-for-user="73357516" type="text/json">{"id":73357516,"first_name":"wes","last_name":"kelly","domain_name":"independent","page_name":"kellywes","display_name":"wes kelly","profile_url":"https://independent.academia.edu/kellywes?f_ri=334552","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_35543978 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="35543978"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 35543978, container: ".js-paper-rank-work_35543978", }); 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$(".js-view-count[data-work-id=35543978]").text(description); $(".js-view-count-work_35543978").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_35543978").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="35543978"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">2</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="47599" href="https://www.academia.edu/Documents/in/Astronomy">Astronomy</a>, <script data-card-contents-for-ri="47599" type="text/json">{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=35543978]'), work: {"id":35543978,"title":"Hubble Revisited on NASA's 50th Anniversary First Confirmation: Planet Kepler-22b An Exoplanet in a Habitable Zone","created_at":"2017-12-30T17:12:25.521-08:00","url":"https://www.academia.edu/35543978/Hubble_Revisited_on_NASAs_50th_Anniversary_First_Confirmation_Planet_Kepler_22b_An_Exoplanet_in_a_Habitable_Zone?f_ri=334552","dom_id":"work_35543978","summary":"One of the earliest identifications of an Earth like extra solar planet was made by the Kepler space observatory in 2012. Designated Kepler 22b, the object was located about 400 light years away near a star slightly cooler and less bright than the sun. The description of the discovery describes the Kepler telescope, the history of planetary transits, the transit of Venus earlier that year - and one of its original observations. ","downloadable_attachments":[{"id":55409486,"asset_id":35543978,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":73357516,"first_name":"wes","last_name":"kelly","domain_name":"independent","page_name":"kellywes","display_name":"wes kelly","profile_url":"https://independent.academia.edu/kellywes?f_ri=334552","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4173924" data-work_id="4173924" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4173924/Extra_Solar_Planetary_Systems_II_Habitable_Planets_in_the_Galaxy">Extra-Solar Planetary Systems II: Habitable Planets in the Galaxy</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">"A lengthy analysis of the output of the "Silicon Creation" model is presented. Seven thousand five hundred microcomputer simulations of stars in the mass range 0.6 - 1.3M⊙ suggest that habitable planets are to be expect to occur around... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4173924" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">"A lengthy analysis of the output of the "Silicon Creation" model is presented. <br />Seven thousand five hundred microcomputer simulations of stars in the mass range 0.6 - 1.3M⊙ suggest that habitable planets are to be expect to occur around stars of between 0.8 - 1.2 M⊙ and most commonly around stars between 0.95 - 1.05 M⊙. The characteristics of these planets range between extremes of mass ~ 0.4 - 2.8 M_e; surface gravity ~ 0.7 - 1.5 g; atmospheric pressure ~ 500 - 2000 mb; average surface temperature ~ 1 C - 21 C; hydrosphere ~ 50 - 99%. <br />An extended simulation of an evolving volume of Galactic disc space, 270 ly in diameter, containing 100,000 star systems of maximum age 10^10 years was performed, assuming constant stellar birthrate and rising metallicity with time. 86 habitable planets were produced giving a value for the ratio of habitable planets to stars in the disc N_HP / N_*disc = 8.6x10^4. The average separation between habitable planets is therefore ~ 50 ly and the number of habitable planets in the Galaxy is approximately 90 million. <br />Comparison of these results is made with those of other authors and uncertainties inherent in the "Silicon Creation" model are briefly discussed."</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4173924" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="8452083cdcb0f63c56fa5461215e5f59" rel="nofollow" data-download="{"attachment_id":31676408,"asset_id":4173924,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31676408/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4173924 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4173924"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4173924, container: ".js-paper-rank-work_4173924", }); });</script></li><li class="js-percentile-work_4173924 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4173924; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4173924"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4173924 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4173924"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4173924; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4173924]").text(description); $(".js-view-count-work_4173924").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4173924").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4173924"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="41236" href="https://www.academia.edu/Documents/in/Extrasolar_planets">Extrasolar planets</a>, <script data-card-contents-for-ri="41236" type="text/json">{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="194384" href="https://www.academia.edu/Documents/in/Planet_Formation">Planet Formation</a><script data-card-contents-for-ri="194384" type="text/json">{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4173924]'), work: {"id":4173924,"title":"Extra-Solar Planetary Systems II: Habitable Planets in the Galaxy","created_at":"2013-08-05T01:31:05.655-07:00","url":"https://www.academia.edu/4173924/Extra_Solar_Planetary_Systems_II_Habitable_Planets_in_the_Galaxy?f_ri=334552","dom_id":"work_4173924","summary":"\"A lengthy analysis of the output of the \"Silicon Creation\" model is presented.\r\nSeven thousand five hundred microcomputer simulations of stars in the mass range 0.6 - 1.3M⊙ suggest that habitable planets are to be expect to occur around stars of between 0.8 - 1.2 M⊙ and most commonly around stars between 0.95 - 1.05 M⊙. The characteristics of these planets range between extremes of mass ~ 0.4 - 2.8 M_e; surface gravity ~ 0.7 - 1.5 g; atmospheric pressure ~ 500 - 2000 mb; average surface temperature ~ 1 C - 21 C; hydrosphere ~ 50 - 99%.\r\nAn extended simulation of an evolving volume of Galactic disc space, 270 ly in diameter, containing 100,000 star systems of maximum age 10^10 years was performed, assuming constant stellar birthrate and rising metallicity with time. 86 habitable planets were produced giving a value for the ratio of habitable planets to stars in the disc N_HP / N_*disc = 8.6x10^4. The average separation between habitable planets is therefore ~ 50 ly and the number of habitable planets in the Galaxy is approximately 90 million.\r\nComparison of these results is made with those of other authors and uncertainties inherent in the \"Silicon Creation\" model are briefly discussed.\"","downloadable_attachments":[{"id":31676408,"asset_id":4173924,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_8943108" data-work_id="8943108" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/8943108/Gomez_Molina_Juan_2014_Review_analogies_and_conjecture_of_the_paper_habitable_zones_of_inhabited_planets_Planetario_Medellin_May_28_">Gomez-Molina Juan (2014) Review, analogies and conjecture of the paper habitable zones of inhabited planets (Planetario Medellin May 28)</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">(Planetario de Medellin, May 28, 6:00-8:30 pm, Group of Astrobiology Ameba <a href="mailto:exobiologia@googlegroups.com" rel="nofollow">exobiologia@googlegroups.com</a>. Attendants: Jorge Zuluaga, Andres Ruiz, Jharley J Garcia Ceren and others). We review critically the paper of Zuluaga JI,... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_8943108" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">(Planetario de Medellin, May 28, 6:00-8:30 pm, Group of Astrobiology Ameba <a href="mailto:exobiologia@googlegroups.com" rel="nofollow">exobiologia@googlegroups.com</a>.  Attendants: Jorge Zuluaga, Andres Ruiz, Jharley J Garcia Ceren and others). <br />  We review critically the paper of Zuluaga JI, Salazar JF Cuartas-Restrepo P and Poveda  G (2014, "The Habitable Zone of Inhabited Planets" arXiv:1405.4576v1) where they discuss the hypothesis that life substantially alters the limits of the habitability zone (HZ) in a planet.  The authors support their hypothesis by computer models (a recent variant of the "Daisyworld", Watson and Lovelock 1983, modified by Lenton, Wood, Salazar and Poveda) and other theoretical arguments.    In order to have a simpler understanding, we present:<br />  1. An electric-circuit analogy for water potential and water flow in a planet.<br />  2. Ball -surface analogies to explain feedbacks, equilibrium states, thresholds, regulation ranges, temperature ranges for liquid water etc.<br />  3. Water-tank analogies to understand the differential equations of the computer model (Forrester JW 1961, Gomez-M, 1993).<br />PERSONAL CONCLUSIONS:<br />1. Biological properties as well as non-biological properties contribute infinitesimally and practically at the same time to the formation of the HZ.<br />2. Conjecture: the more general properties of life in the universe should be described as functions (physiology), not structures (H2O, DNA/RNA etc).  The astrophysiology (Gomez and Restrepo, 2010, sfn.org), a subfield of astrobiology, should do this task.<br />We suspect that:<br />(i) The capacity to generate self-sustained and self-coupled electrical rhythms (regulated at infinitesimal levels) is an esential property of life.<br />(ii) These rhythms are induced and selected for astrophysical events.<br />(abstract written in October 24, 2014).<br /><br />  Se revisa críticamente el articulo de Zuluaga JI, Salazar JF Cuartas-Restrepo P y Poveda G (2014, "la zona habitable de planetas habitados" arXiv: 1405.4576v1) donde discuten la hipótesis de que la vida altera sustancialmente los límites de la Zona de Habitabilidad (ZH) en un planeta. Los autores apoyan su hipótesis con modelos de computadora (una variante reciente del "mundo de las margaritas", Watson y Lovelock 1983, modificado por Lenton, Madera, Salazar y Poveda) y otros argumentos teóricos. Con el fin simplificar y facilitar el entendimiento del articulo, se propuso: <br />  1. Una analogía eléctrica del circuito de potencial de agua y el flujo de agua en un planeta. <br />  2. Analogías bola-superficie para explicar realimentaciones, estados de equilibrio, umbrales, rangos de regulación,  rangos de temperatura para agua líquida, etc <br />  3. Analogías con tanque de agua para entender las ecuaciones diferenciales del modelo de ordenador (Forrester, JW 1961, Gómez-M, 1993). <br />CONCLUSIONES PERSONALES: <br />1. lLas propiedades biológicas, así como las propiedades no biológicos contribuyen infinitesimalmente y prácticamente al mismo tiempo a la formación de la ZH. <br />2. Conjetura: las propiedades más generales de la vida en el universo deben ser descritas como funciones (fisiología), no estructuras (H2O, ADN / ARN, etc).  La astrofisiologia (Gómez y Restrepo 2010, sfn.org), un subcampo de la astrobiologia, debe realizar esta tarea. <br />Tenemos la sospecha de que: <br />(i) La capacidad de generar ritmos eléctricos autosuficientes y auto-acoplados (regulados a niveles infinitesimales) es una propiedad esencial de la vida. <br />(ii) Este ritmos son inducidos y seleccionados por eventos astrofísicos. <br />(resumen escrito el 24 de octubre 2014).</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/8943108" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="881ec58ad18f58d51634df5442d4b737" rel="nofollow" data-download="{"attachment_id":35263595,"asset_id":8943108,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/35263595/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="15867359" href="https://independent.academia.edu/JuanFernandoGomezMolina">Juan-Fernando Gomez-Molina</a><script data-card-contents-for-user="15867359" type="text/json">{"id":15867359,"first_name":"Juan-Fernando","last_name":"Gomez-Molina","domain_name":"independent","page_name":"JuanFernandoGomezMolina","display_name":"Juan-Fernando Gomez-Molina","profile_url":"https://independent.academia.edu/JuanFernandoGomezMolina?f_ri=334552","photo":"https://0.academia-photos.com/15867359/4287537/6182814/s65_juan_fernando.gomez-molina.jpg"}</script></span></span></li><li class="js-paper-rank-work_8943108 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="8943108"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 8943108, container: ".js-paper-rank-work_8943108", }); 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$(".js-view-count[data-work-id=8943108]").text(description); $(".js-view-count-work_8943108").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_8943108").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="8943108"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">7</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="1080" href="https://www.academia.edu/Documents/in/Dynamical_Systems">Dynamical Systems</a>, <script data-card-contents-for-ri="1080" type="text/json">{"id":1080,"name":"Dynamical Systems","url":"https://www.academia.edu/Documents/in/Dynamical_Systems?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="2007" href="https://www.academia.edu/Documents/in/Electrophysiology">Electrophysiology</a>, <script data-card-contents-for-ri="2007" type="text/json">{"id":2007,"name":"Electrophysiology","url":"https://www.academia.edu/Documents/in/Electrophysiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="2215" href="https://www.academia.edu/Documents/in/Water">Water</a>, <script data-card-contents-for-ri="2215" type="text/json">{"id":2215,"name":"Water","url":"https://www.academia.edu/Documents/in/Water?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a><script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=8943108]'), work: {"id":8943108,"title":"Gomez-Molina Juan (2014) Review, analogies and conjecture of the paper habitable zones of inhabited planets (Planetario Medellin May 28)","created_at":"2014-10-24T06:14:55.074-07:00","url":"https://www.academia.edu/8943108/Gomez_Molina_Juan_2014_Review_analogies_and_conjecture_of_the_paper_habitable_zones_of_inhabited_planets_Planetario_Medellin_May_28_?f_ri=334552","dom_id":"work_8943108","summary":"(Planetario de Medellin, May 28, 6:00-8:30 pm, Group of Astrobiology Ameba exobiologia@googlegroups.com. Attendants: Jorge Zuluaga, Andres Ruiz, Jharley J Garcia Ceren and others). \n We review critically the paper of Zuluaga JI, Salazar JF Cuartas-Restrepo P and Poveda G (2014, \"The Habitable Zone of Inhabited Planets\" arXiv:1405.4576v1) where they discuss the hypothesis that life substantially alters the limits of the habitability zone (HZ) in a planet. The authors support their hypothesis by computer models (a recent variant of the \"Daisyworld\", Watson and Lovelock 1983, modified by Lenton, Wood, Salazar and Poveda) and other theoretical arguments. In order to have a simpler understanding, we present:\n 1. An electric-circuit analogy for water potential and water flow in a planet.\n 2. Ball -surface analogies to explain feedbacks, equilibrium states, thresholds, regulation ranges, temperature ranges for liquid water etc.\n 3. Water-tank analogies to understand the differential equations of the computer model (Forrester JW 1961, Gomez-M, 1993).\nPERSONAL CONCLUSIONS:\n1. Biological properties as well as non-biological properties contribute infinitesimally and practically at the same time to the formation of the HZ.\n2. Conjecture: the more general properties of life in the universe should be described as functions (physiology), not structures (H2O, DNA/RNA etc). The astrophysiology (Gomez and Restrepo, 2010, sfn.org), a subfield of astrobiology, should do this task.\nWe suspect that:\n(i) The capacity to generate self-sustained and self-coupled electrical rhythms (regulated at infinitesimal levels) is an esential property of life.\n(ii) These rhythms are induced and selected for astrophysical events.\n(abstract written in October 24, 2014).\n\n Se revisa críticamente el articulo de Zuluaga JI, Salazar JF Cuartas-Restrepo P y Poveda G (2014, \"la zona habitable de planetas habitados\" arXiv: 1405.4576v1) donde discuten la hipótesis de que la vida altera sustancialmente los límites de la Zona de Habitabilidad (ZH) en un planeta. Los autores apoyan su hipótesis con modelos de computadora (una variante reciente del \"mundo de las margaritas\", Watson y Lovelock 1983, modificado por Lenton, Madera, Salazar y Poveda) y otros argumentos teóricos. Con el fin simplificar y facilitar el entendimiento del articulo, se propuso: \n 1. Una analogía eléctrica del circuito de potencial de agua y el flujo de agua en un planeta. \n 2. Analogías bola-superficie para explicar realimentaciones, estados de equilibrio, umbrales, rangos de regulación, rangos de temperatura para agua líquida, etc \n 3. Analogías con tanque de agua para entender las ecuaciones diferenciales del modelo de ordenador (Forrester, JW 1961, Gómez-M, 1993). \nCONCLUSIONES PERSONALES: \n1. lLas propiedades biológicas, así como las propiedades no biológicos contribuyen infinitesimalmente y prácticamente al mismo tiempo a la formación de la ZH. \n2. Conjetura: las propiedades más generales de la vida en el universo deben ser descritas como funciones (fisiología), no estructuras (H2O, ADN / ARN, etc). La astrofisiologia (Gómez y Restrepo 2010, sfn.org), un subcampo de la astrobiologia, debe realizar esta tarea. \nTenemos la sospecha de que: \n(i) La capacidad de generar ritmos eléctricos autosuficientes y auto-acoplados (regulados a niveles infinitesimales) es una propiedad esencial de la vida. \n(ii) Este ritmos son inducidos y seleccionados por eventos astrofísicos. \n(resumen escrito el 24 de octubre 2014).","downloadable_attachments":[{"id":35263595,"asset_id":8943108,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":15867359,"first_name":"Juan-Fernando","last_name":"Gomez-Molina","domain_name":"independent","page_name":"JuanFernandoGomezMolina","display_name":"Juan-Fernando Gomez-Molina","profile_url":"https://independent.academia.edu/JuanFernandoGomezMolina?f_ri=334552","photo":"https://0.academia-photos.com/15867359/4287537/6182814/s65_juan_fernando.gomez-molina.jpg"}],"research_interests":[{"id":1080,"name":"Dynamical Systems","url":"https://www.academia.edu/Documents/in/Dynamical_Systems?f_ri=334552","nofollow":false},{"id":2007,"name":"Electrophysiology","url":"https://www.academia.edu/Documents/in/Electrophysiology?f_ri=334552","nofollow":false},{"id":2215,"name":"Water","url":"https://www.academia.edu/Documents/in/Water?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11820,"name":"Modeling and Simulation","url":"https://www.academia.edu/Documents/in/Modeling_and_Simulation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":1145057,"name":"Daisyworld Model","url":"https://www.academia.edu/Documents/in/Daisyworld_Model?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4174014" data-work_id="4174014" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4174014/Extra_Solar_Planetary_Systems_III_Potential_Sites_for_the_Origin_and_Evolution_of_Technical_Civilisations">Extra-Solar Planetary Systems III: Potential Sites for the Origin and Evolution of Technical Civilisations.</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The probable abundance of planets possessing suitable conditions for the evolution of technologically capable forms of life has been assessed by an analysis of the series of runs of the "Silicon Creation" computer model. An evolutionary... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4174014" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The probable abundance of planets possessing suitable conditions for the evolution of technologically capable forms of life has been assessed by an analysis of the series of runs of the "Silicon Creation" computer model. <br />An evolutionary simulation of 100,000 disc stars of varying mass, metallicity and age was performed. Not only did the computer search for potential civilisation sites, but also for civilisations that had come into existence on those planets over the past 10^10 years of galactic disc history. <br />The frequency of such planets was determined to be N_sites/N_*disc = 2.92x10^-3. The frequency of planets actually developing a technological civilisation was N_civ/N_sites = 0.031, which gives N_civ/N_*disc= 9x10^-5. <br />These figures are two orders of magnitude lower than the most optimistic manipulations of the Drake Equation, but not low enough to resolve the "Fermi Paradox."</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4174014" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="a55b0c492d7f586c5a15337565070900" rel="nofollow" data-download="{"attachment_id":31676477,"asset_id":4174014,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31676477/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4174014 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4174014"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4174014, container: ".js-paper-rank-work_4174014", }); });</script></li><li class="js-percentile-work_4174014 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4174014; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4174014"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4174014 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4174014"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4174014; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4174014]").text(description); $(".js-view-count-work_4174014").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4174014").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4174014"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="36269" href="https://www.academia.edu/Documents/in/Astrosociology_and_Fermi_Paradox">Astrosociology & Fermi Paradox</a>, <script data-card-contents-for-ri="36269" type="text/json">{"id":36269,"name":"Astrosociology \u0026 Fermi Paradox","url":"https://www.academia.edu/Documents/in/Astrosociology_and_Fermi_Paradox?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="36271" href="https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_">SETI (Search for Extraterrestrial Intelligence)</a>, <script data-card-contents-for-ri="36271" type="text/json">{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="41236" href="https://www.academia.edu/Documents/in/Extrasolar_planets">Extrasolar planets</a><script data-card-contents-for-ri="41236" type="text/json">{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4174014]'), work: {"id":4174014,"title":"Extra-Solar Planetary Systems III: Potential Sites for the Origin and Evolution of Technical Civilisations.","created_at":"2013-08-05T01:44:04.879-07:00","url":"https://www.academia.edu/4174014/Extra_Solar_Planetary_Systems_III_Potential_Sites_for_the_Origin_and_Evolution_of_Technical_Civilisations?f_ri=334552","dom_id":"work_4174014","summary":"The probable abundance of planets possessing suitable conditions for the evolution of technologically capable forms of life has been assessed by an analysis of the series of runs of the \"Silicon Creation\" computer model.\r\nAn evolutionary simulation of 100,000 disc stars of varying mass, metallicity and age was performed. Not only did the computer search for potential civilisation sites, but also for civilisations that had come into existence on those planets over the past 10^10 years of galactic disc history.\r\nThe frequency of such planets was determined to be N_sites/N_*disc = 2.92x10^-3. The frequency of planets actually developing a technological civilisation was N_civ/N_sites = 0.031, which gives N_civ/N_*disc= 9x10^-5.\r\nThese figures are two orders of magnitude lower than the most optimistic manipulations of the Drake Equation, but not low enough to resolve the \"Fermi Paradox.\"","downloadable_attachments":[{"id":31676477,"asset_id":4174014,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":36269,"name":"Astrosociology \u0026 Fermi Paradox","url":"https://www.academia.edu/Documents/in/Astrosociology_and_Fermi_Paradox?f_ri=334552","nofollow":false},{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_32892272" data-work_id="32892272" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/32892272/SETI_S_Mission_Impossible_05_07_2017_pdf">SETI’S Mission Impossible 05-07-2017.pdf</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The author argues that the complexity of any extraterrestrial life form that could evolve to the point that it could produce radio signals which could be detected by radio telescopes on Earth is virtually imposible. Using human beings as... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_32892272" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The author argues that the complexity of any extraterrestrial life form that could evolve to the point that it could produce radio signals which could be detected by radio telescopes on Earth is virtually imposible. Using human beings as a proxy, the author challenges the famous Drake Equation used to estimate the likelihood of civilizations on other planets with capabilites similar to ours. As opposed to the Drake Equation’s seven variables, the author identifies 57, but uses only 40, which are assumed to be sequential and thereby calcuable as a factorial. The end result for succession of 40 conditions in order for life like ours to exist on another planet would be 40!, which is 8.16^47. That is to say, the chances of another alien civilization like ours is a little under one in 8.16 trillion, trillion, trillion, trillion. So, clearly, the Search for Extraterrestrial Intelligence is all but impossible.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/32892272" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="05919e5d7e04522f909e3c84f0d00509" rel="nofollow" data-download="{"attachment_id":53032709,"asset_id":32892272,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/53032709/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5262433" href="https://independent.academia.edu/HerbVanFleet">Herb Van Fleet</a><script data-card-contents-for-user="5262433" type="text/json">{"id":5262433,"first_name":"Herb","last_name":"Van Fleet","domain_name":"independent","page_name":"HerbVanFleet","display_name":"Herb Van Fleet","profile_url":"https://independent.academia.edu/HerbVanFleet?f_ri=334552","photo":"https://gravatar.com/avatar/271ef1af6e9f7488ca2300dabfe57d4c?s=65"}</script></span></span></li><li class="js-paper-rank-work_32892272 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="32892272"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 32892272, container: ".js-paper-rank-work_32892272", }); });</script></li><li class="js-percentile-work_32892272 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 32892272; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_32892272"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_32892272 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="32892272"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 32892272; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=32892272]").text(description); $(".js-view-count-work_32892272").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_32892272").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="32892272"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="772" href="https://www.academia.edu/Documents/in/Human_Evolution">Human Evolution</a>, <script data-card-contents-for-ri="772" type="text/json">{"id":772,"name":"Human Evolution","url":"https://www.academia.edu/Documents/in/Human_Evolution?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="36271" href="https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_">SETI (Search for Extraterrestrial Intelligence)</a>, <script data-card-contents-for-ri="36271" type="text/json">{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="61024" href="https://www.academia.edu/Documents/in/Nasa">Nasa</a><script data-card-contents-for-ri="61024" type="text/json">{"id":61024,"name":"Nasa","url":"https://www.academia.edu/Documents/in/Nasa?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=32892272]'), work: {"id":32892272,"title":"SETI’S Mission Impossible 05-07-2017.pdf","created_at":"2017-05-07T11:39:02.458-07:00","url":"https://www.academia.edu/32892272/SETI_S_Mission_Impossible_05_07_2017_pdf?f_ri=334552","dom_id":"work_32892272","summary":"The author argues that the complexity of any extraterrestrial life form that could evolve to the point that it could produce radio signals which could be detected by radio telescopes on Earth is virtually imposible. Using human beings as a proxy, the author challenges the famous Drake Equation used to estimate the likelihood of civilizations on other planets with capabilites similar to ours. As opposed to the Drake Equation’s seven variables, the author identifies 57, but uses only 40, which are assumed to be sequential and thereby calcuable as a factorial. The end result for succession of 40 conditions in order for life like ours to exist on another planet would be 40!, which is 8.16^47. That is to say, the chances of another alien civilization like ours is a little under one in 8.16 trillion, trillion, trillion, trillion. So, clearly, the Search for Extraterrestrial Intelligence is all but impossible. \n","downloadable_attachments":[{"id":53032709,"asset_id":32892272,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5262433,"first_name":"Herb","last_name":"Van Fleet","domain_name":"independent","page_name":"HerbVanFleet","display_name":"Herb Van Fleet","profile_url":"https://independent.academia.edu/HerbVanFleet?f_ri=334552","photo":"https://gravatar.com/avatar/271ef1af6e9f7488ca2300dabfe57d4c?s=65"}],"research_interests":[{"id":772,"name":"Human Evolution","url":"https://www.academia.edu/Documents/in/Human_Evolution?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552","nofollow":false},{"id":61024,"name":"Nasa","url":"https://www.academia.edu/Documents/in/Nasa?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":441848,"name":"Drake equation","url":"https://www.academia.edu/Documents/in/Drake_equation?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_13103147" data-work_id="13103147" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/13103147/Is_there_intelligent_life_out_there">Is there intelligent life out there?</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest">This is a Scientific American article that describes the search for intelligent life in the universe. It was published in 1998</div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/13103147" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="dd5190959da42309ad7fa2b5d2ae4992" rel="nofollow" data-download="{"attachment_id":37945983,"asset_id":13103147,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/37945983/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="31221696" href="https://ajitha.academia.edu/GuillermoLemarchand">Guillermo A . Lemarchand</a><script data-card-contents-for-user="31221696" type="text/json">{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}</script></span></span></li><li class="js-paper-rank-work_13103147 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="13103147"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 13103147, container: ".js-paper-rank-work_13103147", }); });</script></li><li class="js-percentile-work_13103147 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 13103147; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_13103147"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_13103147 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="13103147"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 13103147; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=13103147]").text(description); $(".js-view-count-work_13103147").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_13103147").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="13103147"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="36271" href="https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_">SETI (Search for Extraterrestrial Intelligence)</a>, <script data-card-contents-for-ri="36271" type="text/json">{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="46818" href="https://www.academia.edu/Documents/in/Exobiology">Exobiology</a>, <script data-card-contents-for-ri="46818" type="text/json">{"id":46818,"name":"Exobiology","url":"https://www.academia.edu/Documents/in/Exobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="189148" href="https://www.academia.edu/Documents/in/Radioastronomy">Radioastronomy</a><script data-card-contents-for-ri="189148" type="text/json">{"id":189148,"name":"Radioastronomy","url":"https://www.academia.edu/Documents/in/Radioastronomy?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=13103147]'), work: {"id":13103147,"title":"Is there intelligent life out there?","created_at":"2015-06-19T07:42:23.821-07:00","url":"https://www.academia.edu/13103147/Is_there_intelligent_life_out_there?f_ri=334552","dom_id":"work_13103147","summary":"This is a Scientific American article that describes the search for intelligent life in the universe. It was published in 1998","downloadable_attachments":[{"id":37945983,"asset_id":13103147,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}],"research_interests":[{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552","nofollow":false},{"id":46818,"name":"Exobiology","url":"https://www.academia.edu/Documents/in/Exobiology?f_ri=334552","nofollow":false},{"id":189148,"name":"Radioastronomy","url":"https://www.academia.edu/Documents/in/Radioastronomy?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_11046526" data-work_id="11046526" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/11046526/Habitable_Zones_around_Main_sequence_Stars_New_Estimates">Habitable Zones around Main-sequence Stars: New Estimates</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Identifying terrestrial planets in the habitable zones (HZs) of other stars is one of the primary goals of ongoing radial velocity (RV) and transit exoplanet surveys and proposed future space missions. Most current estimates of the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_11046526" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Identifying terrestrial planets in the habitable zones (HZs) of other stars is one of the primary goals of ongoing radial velocity (RV) and transit exoplanet surveys and proposed future space missions. Most current estimates of the boundaries of the HZ are based on one-dimensional (1D), cloud-free, climate model calculations by Kasting et al. However, this model used band models that were based on older HITRAN and HITEMP line-by-line databases. The inner edge of the HZ in the Kasting et al. model was determined by loss of water, and the outer edge was determined by the maximum greenhouse provided by a CO2 atmosphere. A conservative estimate for the width of the HZ from this model in our solar system is 0.95-1.67 AU. Here an updated 1D radiative-convective, cloud-free climate model is used to obtain new estimates for HZ widths around F, G, K, and M stars. New H2O and CO2 absorption coefficients, derived from the HITRAN 2008 and HITEMP 2010 line-by-line databases, are important improvements to the climate model. According to the new model, the water-loss (inner HZ) and maximum greenhouse (outer HZ) limits for our solar system are at 0.99 and 1.70 AU, respectively, suggesting that the present Earth lies near the inner edge. Additional calculations are performed for stars with effective temperatures between 2600 and 7200 K, and the results are presented in parametric form, making them easy to apply to actual stars. The new model indicates that, near the inner edge of the HZ, there is no clear distinction between runaway greenhouse and water-loss limits for stars with T eff <~ 5000 K, which has implications for ongoing planet searches around K and M stars. To assess the potential habitability of extrasolar terrestrial planets, we propose using stellar flux incident on a planet rather than equilibrium temperature. This removes the dependence on planetary (Bond) albedo, which varies depending on the host star's spectral type. We suggest that conservative estimates of the HZ (water-loss and maximum greenhouse limits) should be used for current RV surveys and Kepler mission to obtain a lower limit on eta⊕, so that future flagship missions like TPF-C and Darwin are not undersized. Our model does not include the radiative effects of clouds; thus, the actual HZ boundaries may extend further in both directions than the estimates just given.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/11046526" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="14d04c17142e1751c65d3ad22dcdddaf" rel="nofollow" data-download="{"attachment_id":36755071,"asset_id":11046526,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/36755071/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="3494" href="https://geosc-psu.academia.edu/RaviKopparapu">Ravi Kopparapu</a><script data-card-contents-for-user="3494" type="text/json">{"id":3494,"first_name":"Ravi","last_name":"Kopparapu","domain_name":"geosc-psu","page_name":"RaviKopparapu","display_name":"Ravi Kopparapu","profile_url":"https://geosc-psu.academia.edu/RaviKopparapu?f_ri=334552","photo":"https://0.academia-photos.com/3494/1191320/4773211/s65_ravi.kopparapu.png"}</script></span></span></li><li class="js-paper-rank-work_11046526 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="11046526"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 11046526, container: ".js-paper-rank-work_11046526", }); });</script></li><li class="js-percentile-work_11046526 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 11046526; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_11046526"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_11046526 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="11046526"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 11046526; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=11046526]").text(description); $(".js-view-count-work_11046526").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_11046526").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="11046526"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="138103" href="https://www.academia.edu/Documents/in/Aliens">Aliens</a>, <script data-card-contents-for-ri="138103" type="text/json">{"id":138103,"name":"Aliens","url":"https://www.academia.edu/Documents/in/Aliens?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a>, <script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="406486" href="https://www.academia.edu/Documents/in/Habitability">Habitability</a><script data-card-contents-for-ri="406486" type="text/json">{"id":406486,"name":"Habitability","url":"https://www.academia.edu/Documents/in/Habitability?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=11046526]'), work: {"id":11046526,"title":"Habitable Zones around Main-sequence Stars: New Estimates","created_at":"2015-02-24T06:49:11.342-08:00","url":"https://www.academia.edu/11046526/Habitable_Zones_around_Main_sequence_Stars_New_Estimates?f_ri=334552","dom_id":"work_11046526","summary":"Identifying terrestrial planets in the habitable zones (HZs) of other stars is one of the primary goals of ongoing radial velocity (RV) and transit exoplanet surveys and proposed future space missions. Most current estimates of the boundaries of the HZ are based on one-dimensional (1D), cloud-free, climate model calculations by Kasting et al. However, this model used band models that were based on older HITRAN and HITEMP line-by-line databases. The inner edge of the HZ in the Kasting et al. model was determined by loss of water, and the outer edge was determined by the maximum greenhouse provided by a CO2 atmosphere. A conservative estimate for the width of the HZ from this model in our solar system is 0.95-1.67 AU. Here an updated 1D radiative-convective, cloud-free climate model is used to obtain new estimates for HZ widths around F, G, K, and M stars. New H2O and CO2 absorption coefficients, derived from the HITRAN 2008 and HITEMP 2010 line-by-line databases, are important improvements to the climate model. According to the new model, the water-loss (inner HZ) and maximum greenhouse (outer HZ) limits for our solar system are at 0.99 and 1.70 AU, respectively, suggesting that the present Earth lies near the inner edge. Additional calculations are performed for stars with effective temperatures between 2600 and 7200 K, and the results are presented in parametric form, making them easy to apply to actual stars. The new model indicates that, near the inner edge of the HZ, there is no clear distinction between runaway greenhouse and water-loss limits for stars with T eff \u003c~ 5000 K, which has implications for ongoing planet searches around K and M stars. To assess the potential habitability of extrasolar terrestrial planets, we propose using stellar flux incident on a planet rather than equilibrium temperature. This removes the dependence on planetary (Bond) albedo, which varies depending on the host star's spectral type. We suggest that conservative estimates of the HZ (water-loss and maximum greenhouse limits) should be used for current RV surveys and Kepler mission to obtain a lower limit on eta⊕, so that future flagship missions like TPF-C and Darwin are not undersized. Our model does not include the radiative effects of clouds; thus, the actual HZ boundaries may extend further in both directions than the estimates just given.\r\n","downloadable_attachments":[{"id":36755071,"asset_id":11046526,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":3494,"first_name":"Ravi","last_name":"Kopparapu","domain_name":"geosc-psu","page_name":"RaviKopparapu","display_name":"Ravi Kopparapu","profile_url":"https://geosc-psu.academia.edu/RaviKopparapu?f_ri=334552","photo":"https://0.academia-photos.com/3494/1191320/4773211/s65_ravi.kopparapu.png"}],"research_interests":[{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":138103,"name":"Aliens","url":"https://www.academia.edu/Documents/in/Aliens?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":406486,"name":"Habitability","url":"https://www.academia.edu/Documents/in/Habitability?f_ri=334552","nofollow":false},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_18315903" data-work_id="18315903" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/18315903/Deliberate_destruction_of_planets_and_biospheres">Deliberate destruction of planets and biospheres</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Poster's note : discusses the potential for hostile use of geoengineering technologies in interplanetary warfare. Preview available, showing most of the article text. <a href="http://www.jbis.org.uk/paper.php?p=2015.68.150" rel="nofollow">http://www.jbis.org.uk/paper.php?p=2015.68.150</a> Deliberate Destruction... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_18315903" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Poster's note : discusses the potential for hostile use of geoengineering technologies in interplanetary warfare. Preview available, showing most of the article text.<br /><br /><a href="http://www.jbis.org.uk/paper.php?p=2015.68.150" rel="nofollow">http://www.jbis.org.uk/paper.php?p=2015.68.150</a><br />Deliberate Destruction of Planets and Biospheres<br />Science fiction offers scenarios in which a planet is destroyed in combat. However, these are often impractical. Instead of supplying all the energy required, more plausible attacks may use leverage in order to damage or destroy the planet or its biosphere. In order to study the conduct, observation, or defence associated with such attacks, a range of potentially practical weapon and defence technologies are discussed. These are: altering the radiation budget of a planet so as to substantially change its temperature; introducing invasive species to transform the biogeochemistry; and using orbital perturbations of comets and asteroids to cause collisions, or to move the planet to an unstable or uninhabitable orbit. Weapon transit and effect times associated with these technologies render them suitable only for extreme slow-motion warfare, assuming near-term technologies.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/18315903" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="6670f131c7b31ce54683de723e02e4df" rel="nofollow" data-download="{"attachment_id":52887566,"asset_id":18315903,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/52887566/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="16446192" href="https://ucl.academia.edu/AndrewLockley">Andrew Lockley</a><script data-card-contents-for-user="16446192" type="text/json">{"id":16446192,"first_name":"Andrew","last_name":"Lockley","domain_name":"ucl","page_name":"AndrewLockley","display_name":"Andrew Lockley","profile_url":"https://ucl.academia.edu/AndrewLockley?f_ri=334552","photo":"https://0.academia-photos.com/16446192/4478962/35481100/s65_andrew.lockley.jpg"}</script></span></span></li><li class="js-paper-rank-work_18315903 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="18315903"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 18315903, container: ".js-paper-rank-work_18315903", }); });</script></li><li class="js-percentile-work_18315903 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 18315903; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_18315903"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_18315903 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="18315903"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 18315903; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=18315903]").text(description); $(".js-view-count-work_18315903").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_18315903").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="18315903"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">13</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a>, <script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="39280" href="https://www.academia.edu/Documents/in/Ethics_of_Geoengineering">Ethics of Geoengineering</a><script data-card-contents-for-ri="39280" type="text/json">{"id":39280,"name":"Ethics of Geoengineering","url":"https://www.academia.edu/Documents/in/Ethics_of_Geoengineering?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=18315903]'), work: {"id":18315903,"title":"Deliberate destruction of planets and biospheres","created_at":"2015-11-14T01:15:29.979-08:00","url":"https://www.academia.edu/18315903/Deliberate_destruction_of_planets_and_biospheres?f_ri=334552","dom_id":"work_18315903","summary":"Poster's note : discusses the potential for hostile use of geoengineering technologies in interplanetary warfare. Preview available, showing most of the article text.\n\nhttp://www.jbis.org.uk/paper.php?p=2015.68.150\nDeliberate Destruction of Planets and Biospheres\nScience fiction offers scenarios in which a planet is destroyed in combat. However, these are often impractical. Instead of supplying all the energy required, more plausible attacks may use leverage in order to damage or destroy the planet or its biosphere. In order to study the conduct, observation, or defence associated with such attacks, a range of potentially practical weapon and defence technologies are discussed. These are: altering the radiation budget of a planet so as to substantially change its temperature; introducing invasive species to transform the biogeochemistry; and using orbital perturbations of comets and asteroids to cause collisions, or to move the planet to an unstable or uninhabitable orbit. Weapon transit and effect times associated with these technologies render them suitable only for extreme slow-motion warfare, assuming near-term technologies. ","downloadable_attachments":[{"id":52887566,"asset_id":18315903,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":16446192,"first_name":"Andrew","last_name":"Lockley","domain_name":"ucl","page_name":"AndrewLockley","display_name":"Andrew Lockley","profile_url":"https://ucl.academia.edu/AndrewLockley?f_ri=334552","photo":"https://0.academia-photos.com/16446192/4478962/35481100/s65_andrew.lockley.jpg"}],"research_interests":[{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":39280,"name":"Ethics of Geoengineering","url":"https://www.academia.edu/Documents/in/Ethics_of_Geoengineering?f_ri=334552","nofollow":false},{"id":39286,"name":"Exoplanet detection","url":"https://www.academia.edu/Documents/in/Exoplanet_detection?f_ri=334552"},{"id":93753,"name":"Geoengineering","url":"https://www.academia.edu/Documents/in/Geoengineering?f_ri=334552"},{"id":138103,"name":"Aliens","url":"https://www.academia.edu/Documents/in/Aliens?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":359268,"name":"Sustainability, geoengineering, climate justice","url":"https://www.academia.edu/Documents/in/Sustainability_geoengineering_climate_justice?f_ri=334552"},{"id":590234,"name":"Marine Geoengineering","url":"https://www.academia.edu/Documents/in/Marine_Geoengineering?f_ri=334552"},{"id":701140,"name":"Geoengineering/Climate Engineering","url":"https://www.academia.edu/Documents/in/Geoengineering_Climate_Engineering?f_ri=334552"},{"id":974606,"name":"Astrobiology/Exobiology","url":"https://www.academia.edu/Documents/in/Astrobiology_Exobiology?f_ri=334552"},{"id":1345418,"name":"Geoengineering and Weather Modification","url":"https://www.academia.edu/Documents/in/Geoengineering_and_Weather_Modification?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_49638699 coauthored" data-work_id="49638699" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/49638699/Indexing_of_exoplanets_in_search_for_potential_habitability_application_to_Mars_like_worlds">Indexing of exoplanets in search for potential habitability: application to Mars-like worlds</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Study of exoplanets is one of the main goals of present research in planetary sciences and astrobiology. Analysis of huge planetary data from space missions such as CoRoT and Kepler is directed ultimately at finding a planet similar to... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_49638699" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Study of exoplanets is one of the main goals of present research in planetary sciences and astrobiology. Analysis of huge planetary data from space missions such as CoRoT and Kepler is directed ultimately at finding a planet similar to Earth—the Earth&#39;s twin, and answering the question of potential exo-habitability. The Earth Similarity Index (ESI) is a first step in this quest, ranging from 1 (Earth) to 0 (totally dissimilar to Earth). It was defined for the four physical parameters of a planet: radius, density, escape velocity and surface temperature. The ESI is further subdivided into interior ESI (geometrical mean of radius and density) and surface ESI (geometrical mean of escape velocity and surface temperature). The challenge here is to determine which exoplanet parameter(s) is important in finding this similarity ; how exactly the individual parameters entering the interior ESI and surface ESI are contributing to the global ESI. Since the surface temperature entering surf...</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/49638699" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="496c8783c6c5453c703fd98301e7b51a" rel="nofollow" data-download="{"attachment_id":67940141,"asset_id":49638699,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/67940141/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="86918346" href="https://iiap.academia.edu/Safonova">Margarita Safonova</a><script data-card-contents-for-user="86918346" type="text/json">{"id":86918346,"first_name":"Margarita","last_name":"Safonova","domain_name":"iiap","page_name":"Safonova","display_name":"Margarita Safonova","profile_url":"https://iiap.academia.edu/Safonova?f_ri=334552","photo":"https://0.academia-photos.com/86918346/29565158/27501991/s65_margarita.safonova.jpg"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-49638699">+1</span><div class="hidden js-additional-users-49638699"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://christuniversity.academia.edu/ShivappaGudennavar">Shivappa Gudennavar</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-49638699'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-49638699').html(); } } new HoverPopover(popoverSettings); })();</script></li><li class="js-paper-rank-work_49638699 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="49638699"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 49638699, container: ".js-paper-rank-work_49638699", }); });</script></li><li class="js-percentile-work_49638699 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 49638699; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_49638699"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_49638699 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="49638699"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 49638699; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=49638699]").text(description); $(".js-view-count-work_49638699").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_49638699").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="49638699"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">2</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a>, <script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="406486" href="https://www.academia.edu/Documents/in/Habitability">Habitability</a><script data-card-contents-for-ri="406486" type="text/json">{"id":406486,"name":"Habitability","url":"https://www.academia.edu/Documents/in/Habitability?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=49638699]'), work: {"id":49638699,"title":"Indexing of exoplanets in search for potential habitability: application to Mars-like worlds","created_at":"2021-07-09T03:45:04.853-07:00","url":"https://www.academia.edu/49638699/Indexing_of_exoplanets_in_search_for_potential_habitability_application_to_Mars_like_worlds?f_ri=334552","dom_id":"work_49638699","summary":"Study of exoplanets is one of the main goals of present research in planetary sciences and astrobiology. Analysis of huge planetary data from space missions such as CoRoT and Kepler is directed ultimately at finding a planet similar to Earth—the Earth\u0026#39;s twin, and answering the question of potential exo-habitability. The Earth Similarity Index (ESI) is a first step in this quest, ranging from 1 (Earth) to 0 (totally dissimilar to Earth). It was defined for the four physical parameters of a planet: radius, density, escape velocity and surface temperature. The ESI is further subdivided into interior ESI (geometrical mean of radius and density) and surface ESI (geometrical mean of escape velocity and surface temperature). The challenge here is to determine which exoplanet parameter(s) is important in finding this similarity ; how exactly the individual parameters entering the interior ESI and surface ESI are contributing to the global ESI. Since the surface temperature entering surf...","downloadable_attachments":[{"id":67940141,"asset_id":49638699,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":86918346,"first_name":"Margarita","last_name":"Safonova","domain_name":"iiap","page_name":"Safonova","display_name":"Margarita Safonova","profile_url":"https://iiap.academia.edu/Safonova?f_ri=334552","photo":"https://0.academia-photos.com/86918346/29565158/27501991/s65_margarita.safonova.jpg"},{"id":10568050,"first_name":"Shivappa","last_name":"Gudennavar","domain_name":"christuniversity","page_name":"ShivappaGudennavar","display_name":"Shivappa Gudennavar","profile_url":"https://christuniversity.academia.edu/ShivappaGudennavar?f_ri=334552","photo":"https://0.academia-photos.com/10568050/7421083/8341216/s65_shivappa.b..gudennavar.jpg"}],"research_interests":[{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":406486,"name":"Habitability","url":"https://www.academia.edu/Documents/in/Habitability?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_40199106" data-work_id="40199106" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/40199106/THE_ASTRODYNAMICS_OF_NEW_PLANETARY_SYSTEMS_THE_ELLIPTIC_RESTRICTED_3_BODY_PROBLEM">THE ASTRODYNAMICS OF NEW PLANETARY SYSTEMS: THE ELLIPTIC RESTRICTED 3-BODY PROBLEM</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Elliptic Restricted 3-Body Problem (ER3BP) simulations illustrate measures of relative stability for extra-solar planets, using terrestrial analogs as 3rd bodies in binary systems Centauri, Procyon, Sirius, Jupiter-Sun, 47 Ursae Majoris... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_40199106" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Elliptic Restricted 3-Body Problem (ER3BP) simulations illustrate measures of relative stability for extra-solar planets, using terrestrial analogs as 3rd bodies in binary systems Centauri, Procyon, Sirius, Jupiter-Sun, 47 Ursae Majoris and 70 Virginis. Initial conditions placed hypothetical planets in nominally circular orbits at Earth analogous radiative flux regions (400 o K effective stellar temperature at orbital radius), plus increments above and below. As tracked for 10 3-10 5 years, secondary bodies (star, brown dwarf or planet) perturbed nominally circular, co-planar planetary orbits at pericentron passage, causing eccentricity and angular momentum to cycle from 10 2 to 10 5 years as planet periastron precessed. Cases include satellites of jovian planets or brown dwarfs. Cycle magnitudes and periods varied with star system case and thermal environment. In some instances, stable orbit bounds were established by capture, ejection or advent of chaotic motions. Effective temperature bounds of stable regions varied with each binary system. For calibrating detection projects, observations of Earth from deep space are suggested.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/40199106" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="237e2e856d2698604fb422241def420f" rel="nofollow" data-download="{"attachment_id":60424594,"asset_id":40199106,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/60424594/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="58251247" href="https://independent.academia.edu/weskelly">wes kelly</a><script data-card-contents-for-user="58251247" type="text/json">{"id":58251247,"first_name":"wes","last_name":"kelly","domain_name":"independent","page_name":"weskelly","display_name":"wes kelly","profile_url":"https://independent.academia.edu/weskelly?f_ri=334552","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_40199106 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="40199106"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 40199106, container: ".js-paper-rank-work_40199106", }); });</script></li><li class="js-percentile-work_40199106 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 40199106; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_40199106"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_40199106 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="40199106"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 40199106; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=40199106]").text(description); $(".js-view-count-work_40199106").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_40199106").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="40199106"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i></div><span class="InlineList-item-text u-textTruncate u-pl6x"><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (false) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=40199106]'), work: {"id":40199106,"title":"THE ASTRODYNAMICS OF NEW PLANETARY SYSTEMS: THE ELLIPTIC RESTRICTED 3-BODY PROBLEM","created_at":"2019-08-28T14:21:22.525-07:00","url":"https://www.academia.edu/40199106/THE_ASTRODYNAMICS_OF_NEW_PLANETARY_SYSTEMS_THE_ELLIPTIC_RESTRICTED_3_BODY_PROBLEM?f_ri=334552","dom_id":"work_40199106","summary":"Elliptic Restricted 3-Body Problem (ER3BP) simulations illustrate measures of relative stability for extra-solar planets, using terrestrial analogs as 3rd bodies in binary systems Centauri, Procyon, Sirius, Jupiter-Sun, 47 Ursae Majoris and 70 Virginis. Initial conditions placed hypothetical planets in nominally circular orbits at Earth analogous radiative flux regions (400 o K effective stellar temperature at orbital radius), plus increments above and below. As tracked for 10 3-10 5 years, secondary bodies (star, brown dwarf or planet) perturbed nominally circular, co-planar planetary orbits at pericentron passage, causing eccentricity and angular momentum to cycle from 10 2 to 10 5 years as planet periastron precessed. Cases include satellites of jovian planets or brown dwarfs. Cycle magnitudes and periods varied with star system case and thermal environment. In some instances, stable orbit bounds were established by capture, ejection or advent of chaotic motions. Effective temperature bounds of stable regions varied with each binary system. For calibrating detection projects, observations of Earth from deep space are suggested.","downloadable_attachments":[{"id":60424594,"asset_id":40199106,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":58251247,"first_name":"wes","last_name":"kelly","domain_name":"independent","page_name":"weskelly","display_name":"wes kelly","profile_url":"https://independent.academia.edu/weskelly?f_ri=334552","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_36172875" data-work_id="36172875" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/36172875/Atmospheric_dynamics_and_habitability_range_in_Earth_like_aquaplanets_obliquity_simulations">Atmospheric dynamics and habitability range in Earth-like aquaplanets obliquity simulations</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We present the evolution of the atmospheric variables that affect planetary climate by increasing the obliquity by using a general circulation model (PlaSim) coupled to a slab ocean with mixed layer flux correction. We increase the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_36172875" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present the evolution of the atmospheric variables that affect planetary climate by increasing the obliquity by using a general circulation model (PlaSim) coupled to a slab ocean with mixed layer flux correction. We increase the obliquity between 30 • and 90 • in 16 aquaplanets with liquid sea surface and perform the simulation allowing the sea ice cover formation to be a consequence of its atmospheric dynamics. Insolation is maintained constant in each experiment, but changing the obliquity affects the radiation budget and the large scale circulation. Earth-like atmospheric dynamics is observed for planets with obliquity under 54 •. Above this value, the latitudinal temperature gradient is reversed giving place to a new regime of jet streams, affecting the shape of Hadley and Ferrel cells and changing the position of the InterTropical Convergence Zone. As humidity and high temperatures determine Earth's habitability, we introduce the wet bulb temperature as an atmospheric index of habitability for Earth-like aquaplanets with above freezing temperatures. The aquaplanets are habitable all year round at all latitudes for values under 54 • ; above this value habitability decreases toward the poles due to high temperatures.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/36172875" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="1cd5a97e731ba949c4d320879326614f" rel="nofollow" data-download="{"attachment_id":56071076,"asset_id":36172875,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/56071076/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="45085646" href="https://independent.academia.edu/PriscillaNowajewski">Priscilla Nowajewski</a><script data-card-contents-for-user="45085646" type="text/json">{"id":45085646,"first_name":"Priscilla","last_name":"Nowajewski","domain_name":"independent","page_name":"PriscillaNowajewski","display_name":"Priscilla Nowajewski","profile_url":"https://independent.academia.edu/PriscillaNowajewski?f_ri=334552","photo":"https://0.academia-photos.com/45085646/19287909/19217906/s65_priscilla.nowajewski.png"}</script></span></span></li><li class="js-paper-rank-work_36172875 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="36172875"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 36172875, container: ".js-paper-rank-work_36172875", }); });</script></li><li class="js-percentile-work_36172875 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 36172875; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_36172875"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_36172875 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="36172875"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 36172875; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=36172875]").text(description); $(".js-view-count-work_36172875").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_36172875").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="36172875"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="409" href="https://www.academia.edu/Documents/in/Geophysics">Geophysics</a>, <script data-card-contents-for-ri="409" type="text/json">{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="98914" href="https://www.academia.edu/Documents/in/Meteorology_and_Climatology">Meteorology & Climatology</a>, <script data-card-contents-for-ri="98914" type="text/json">{"id":98914,"name":"Meteorology \u0026 Climatology","url":"https://www.academia.edu/Documents/in/Meteorology_and_Climatology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=36172875]'), work: {"id":36172875,"title":"Atmospheric dynamics and habitability range in Earth-like aquaplanets obliquity simulations","created_at":"2018-03-15T12:09:08.560-07:00","url":"https://www.academia.edu/36172875/Atmospheric_dynamics_and_habitability_range_in_Earth_like_aquaplanets_obliquity_simulations?f_ri=334552","dom_id":"work_36172875","summary":"We present the evolution of the atmospheric variables that affect planetary climate by increasing the obliquity by using a general circulation model (PlaSim) coupled to a slab ocean with mixed layer flux correction. We increase the obliquity between 30 • and 90 • in 16 aquaplanets with liquid sea surface and perform the simulation allowing the sea ice cover formation to be a consequence of its atmospheric dynamics. Insolation is maintained constant in each experiment, but changing the obliquity affects the radiation budget and the large scale circulation. Earth-like atmospheric dynamics is observed for planets with obliquity under 54 •. Above this value, the latitudinal temperature gradient is reversed giving place to a new regime of jet streams, affecting the shape of Hadley and Ferrel cells and changing the position of the InterTropical Convergence Zone. As humidity and high temperatures determine Earth's habitability, we introduce the wet bulb temperature as an atmospheric index of habitability for Earth-like aquaplanets with above freezing temperatures. The aquaplanets are habitable all year round at all latitudes for values under 54 • ; above this value habitability decreases toward the poles due to high temperatures.","downloadable_attachments":[{"id":56071076,"asset_id":36172875,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":45085646,"first_name":"Priscilla","last_name":"Nowajewski","domain_name":"independent","page_name":"PriscillaNowajewski","display_name":"Priscilla Nowajewski","profile_url":"https://independent.academia.edu/PriscillaNowajewski?f_ri=334552","photo":"https://0.academia-photos.com/45085646/19287909/19217906/s65_priscilla.nowajewski.png"}],"research_interests":[{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":98914,"name":"Meteorology \u0026 Climatology","url":"https://www.academia.edu/Documents/in/Meteorology_and_Climatology?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":2638495,"name":"Exoplanet Atmospheres","url":"https://www.academia.edu/Documents/in/Exoplanet_Atmospheres?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4156602" data-work_id="4156602" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4156602/On_the_formation_of_terrestrial_planets_in_hot_Jupiter_systems">On the formation of terrestrial planets in hot-Jupiter systems</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">"Context. There are numerous extrasolar giant planets which orbit close to their central stars. These “hot-Jupiters” probably formed in the outer, cooler regions of their protoplanetary disks, and migrated inward to ∼0.1 AU. Since these... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4156602" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">"Context. There are numerous extrasolar giant planets which orbit close to their central stars. These “hot-Jupiters” probably formed in the outer, cooler regions of their protoplanetary disks, and migrated inward to ∼0.1 AU. Since these giant planets must have migrated through their inner systems at an early time, it is uncertain whether they could have formed or retained terrestrial planets. <br />Aims. We present a series of calculations aimed at examining how an inner system of planetesimals/protoplanets, undergoing terrestrial planet formation, evolves under the influence of a giant planet undergoing inward type II migration through the region bounded between 5–0.1 AU. <br />Methods. We have previously simulated the effect of gas giant planet migration on an inner system protoplanet/planetesimal disk using a N-body code which included gas drag and a prescribed migration rate. We update our calculations here with an improved model that incorporates a viscously evolving gas disk, annular gap and inner-cavity formation due to the gravitational field of the giant planet, and self-consistent evolution of the giant’s orbit. <br />Results. We find that 60% of the solids disk survives by being scattered by the giant planet into external orbits. Planetesimals are scattered outward almost as efficiently as protoplanets, resulting in the regeneration of a solids disk where dynamical friction is strong and terrestrial planet formation is able to resume. A simulation that was extended for a few Myr after the migration of the giant planet halted at 0.1 AU, resulted in an apparently stable planet of ∼2 m⊕ forming in the habitable zone. Migration–induced mixing of volatile-rich material from beyond the “snowline” into the inner disk regions means that terrestrial planets that form there are likely to be water-rich. <br />Conclusions. We predict that hot-Jupiter systems are likely to harbor water-abundant terrestrial planets in their habitable zones. These planets may be detected by future planet search missions."</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4156602" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="42ec42a4693b8d23829ffcca51ce4809" rel="nofollow" data-download="{"attachment_id":31663099,"asset_id":4156602,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31663099/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4156602 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4156602"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4156602, container: ".js-paper-rank-work_4156602", }); });</script></li><li class="js-percentile-work_4156602 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4156602; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4156602"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4156602 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4156602"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4156602; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4156602]").text(description); $(".js-view-count-work_4156602").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4156602").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4156602"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a><script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4156602]'), work: {"id":4156602,"title":"On the formation of terrestrial planets in hot-Jupiter systems","created_at":"2013-08-01T18:31:25.879-07:00","url":"https://www.academia.edu/4156602/On_the_formation_of_terrestrial_planets_in_hot_Jupiter_systems?f_ri=334552","dom_id":"work_4156602","summary":"\"Context. There are numerous extrasolar giant planets which orbit close to their central stars. These “hot-Jupiters” probably formed in the outer, cooler regions of their protoplanetary disks, and migrated inward to ∼0.1 AU. Since these giant planets must have migrated through their inner systems at an early time, it is uncertain whether they could have formed or retained terrestrial planets.\r\nAims. We present a series of calculations aimed at examining how an inner system of planetesimals/protoplanets, undergoing terrestrial planet formation, evolves under the influence of a giant planet undergoing inward type II migration through the region bounded between 5–0.1 AU.\r\nMethods. We have previously simulated the effect of gas giant planet migration on an inner system protoplanet/planetesimal disk using a N-body code which included gas drag and a prescribed migration rate. We update our calculations here with an improved model that incorporates a viscously evolving gas disk, annular gap and inner-cavity formation due to the gravitational field of the giant planet, and self-consistent evolution of the giant’s orbit.\r\nResults. We find that \u000160% of the solids disk survives by being scattered by the giant planet into external orbits. Planetesimals are scattered outward almost as efficiently as protoplanets, resulting in the regeneration of a solids disk where dynamical friction is strong and terrestrial planet formation is able to resume. A simulation that was extended for a few Myr after the migration of the giant planet halted at 0.1 AU, resulted in an apparently stable planet of ∼2 m⊕ forming in the habitable zone. Migration–induced mixing of volatile-rich material from beyond the “snowline” into the inner disk regions means that terrestrial planets that form there are likely to be water-rich.\r\nConclusions. We predict that hot-Jupiter systems are likely to harbor water-abundant terrestrial planets in their habitable zones. These planets may be detected by future planet search missions.\"","downloadable_attachments":[{"id":31663099,"asset_id":4156602,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_74669313" data-work_id="74669313" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/74669313/The_DNA_States_of_Micro_entropy">The DNA States of Micro-entropy</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Images generated by this particular algorithm are not just a better way to represent RNA and DNA and study their formal properties but, as I mentioned before, these are most likely some kind of reflections of the earliest „images of the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_74669313" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Images generated by this particular algorithm are not just a better way to represent RNA and DNA and study their formal properties but, as I mentioned before, these are most likely some kind of reflections of the earliest „images of the world“ as „perceived“ and „remembered“ by life, since the earliest living molecule(the first life). It could also be that these images are in some way expressions of certain properties of all possible life forms including extraterrestrial, that are not based on RNA/DNA, if such entities exist somewhere in the Universe. Whatever their nature might be, those nonorganic living forms in some way have to relate to their environment, at least by being able to distinguish hot from cold, light from dark.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/74669313" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="d979ea78ff5b1848753376f7f756c132" rel="nofollow" data-download="{"attachment_id":82737994,"asset_id":74669313,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/82737994/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="112085808" href="https://independent.academia.edu/GregorMobius">Gregor Mobius</a><script data-card-contents-for-user="112085808" type="text/json">{"id":112085808,"first_name":"Gregor","last_name":"Mobius","domain_name":"independent","page_name":"GregorMobius","display_name":"Gregor Mobius","profile_url":"https://independent.academia.edu/GregorMobius?f_ri=334552","photo":"https://0.academia-photos.com/112085808/44251173/34937532/s65_gregor.mobius.jpg"}</script></span></span></li><li class="js-paper-rank-work_74669313 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="74669313"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 74669313, container: ".js-paper-rank-work_74669313", }); });</script></li><li class="js-percentile-work_74669313 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 74669313; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_74669313"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_74669313 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="74669313"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 74669313; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=74669313]").text(description); $(".js-view-count-work_74669313").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_74669313").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="74669313"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4315" href="https://www.academia.edu/Documents/in/Origins_of_Life">Origins of Life</a>, <script data-card-contents-for-ri="4315" type="text/json">{"id":4315,"name":"Origins of Life","url":"https://www.academia.edu/Documents/in/Origins_of_Life?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="17429" href="https://www.academia.edu/Documents/in/Structural_Bioinformatics">Structural Bioinformatics</a>, <script data-card-contents-for-ri="17429" type="text/json">{"id":17429,"name":"Structural Bioinformatics","url":"https://www.academia.edu/Documents/in/Structural_Bioinformatics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="68656" href="https://www.academia.edu/Documents/in/Biosphere">Biosphere</a>, <script data-card-contents-for-ri="68656" type="text/json">{"id":68656,"name":"Biosphere","url":"https://www.academia.edu/Documents/in/Biosphere?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=74669313]'), work: {"id":74669313,"title":"The DNA States of Micro-entropy","created_at":"2022-03-27T00:36:41.169-07:00","url":"https://www.academia.edu/74669313/The_DNA_States_of_Micro_entropy?f_ri=334552","dom_id":"work_74669313","summary":"Images generated by this particular algorithm are not just a better way to represent RNA and DNA and study their formal properties but, as I mentioned before, these are most likely some kind of reflections of the earliest „images of the world“ as „perceived“ and „remembered“ by life, since the earliest living molecule(the first life). It could also be that these images are in some way expressions of certain properties of all possible life forms including extraterrestrial, that are not based on RNA/DNA, if such entities exist somewhere in the Universe. Whatever their nature might be, those nonorganic living forms in some way have to relate to their environment, at least by being able to distinguish hot from cold, light from dark.","downloadable_attachments":[{"id":82737994,"asset_id":74669313,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":112085808,"first_name":"Gregor","last_name":"Mobius","domain_name":"independent","page_name":"GregorMobius","display_name":"Gregor Mobius","profile_url":"https://independent.academia.edu/GregorMobius?f_ri=334552","photo":"https://0.academia-photos.com/112085808/44251173/34937532/s65_gregor.mobius.jpg"}],"research_interests":[{"id":4315,"name":"Origins of Life","url":"https://www.academia.edu/Documents/in/Origins_of_Life?f_ri=334552","nofollow":false},{"id":17429,"name":"Structural Bioinformatics","url":"https://www.academia.edu/Documents/in/Structural_Bioinformatics?f_ri=334552","nofollow":false},{"id":68656,"name":"Biosphere","url":"https://www.academia.edu/Documents/in/Biosphere?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":3660398,"name":"DNA visualization","url":"https://www.academia.edu/Documents/in/DNA_visualization?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_72964584" data-work_id="72964584" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/72964584/Ultraviolet_radiation_constraints_around_the_circumstellar_habitable_zones">Ultraviolet radiation constraints around the circumstellar habitable zones</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between 200 and 300 nm becomes energetically very damaging to most of... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_72964584" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between 200 and 300 nm becomes energetically very damaging to most of the terrestrial biological systems. On the other hand, UV radiation is usually considered one of the most important energy source on the primitive Earth for the synthesis of many biochemical compounds and, therefore, essential for several biogenesis processes. In this work, we use these properties of the UV radiation to define the boundaries of an ultraviolet habitable zone. We also analyze the evolution of the UV habitable zone during the main sequence stage of the star. We apply these criteria to study the UV habitable zone for those extrasolar planetary systems that were observed by the International Ultraviolet Explorer (IUE). We analyze the possibility that extrasolar planets and moons could be suitable for life, according to the UV constrains ...</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/72964584" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="5a7fdb599d2396d7af5e0e8c5fb8ed92" rel="nofollow" data-download="{"attachment_id":81675998,"asset_id":72964584,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/81675998/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="152571801" href="https://independent.academia.edu/AndreaBuccino">Andrea Buccino</a><script data-card-contents-for-user="152571801" type="text/json">{"id":152571801,"first_name":"Andrea","last_name":"Buccino","domain_name":"independent","page_name":"AndreaBuccino","display_name":"Andrea Buccino","profile_url":"https://independent.academia.edu/AndreaBuccino?f_ri=334552","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_72964584 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="72964584"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 72964584, container: ".js-paper-rank-work_72964584", }); });</script></li><li class="js-percentile-work_72964584 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 72964584; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_72964584"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_72964584 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="72964584"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 72964584; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=72964584]").text(description); $(".js-view-count-work_72964584").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_72964584").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="72964584"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">20</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="407" href="https://www.academia.edu/Documents/in/Geochemistry">Geochemistry</a>, <script data-card-contents-for-ri="407" type="text/json">{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="409" href="https://www.academia.edu/Documents/in/Geophysics">Geophysics</a>, <script data-card-contents-for-ri="409" type="text/json">{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a><script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=72964584]'), work: {"id":72964584,"title":"Ultraviolet radiation constraints around the circumstellar habitable zones","created_at":"2022-03-03T15:36:34.422-08:00","url":"https://www.academia.edu/72964584/Ultraviolet_radiation_constraints_around_the_circumstellar_habitable_zones?f_ri=334552","dom_id":"work_72964584","summary":"Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between 200 and 300 nm becomes energetically very damaging to most of the terrestrial biological systems. On the other hand, UV radiation is usually considered one of the most important energy source on the primitive Earth for the synthesis of many biochemical compounds and, therefore, essential for several biogenesis processes. In this work, we use these properties of the UV radiation to define the boundaries of an ultraviolet habitable zone. We also analyze the evolution of the UV habitable zone during the main sequence stage of the star. We apply these criteria to study the UV habitable zone for those extrasolar planetary systems that were observed by the International Ultraviolet Explorer (IUE). We analyze the possibility that extrasolar planets and moons could be suitable for life, according to the UV constrains ...","downloadable_attachments":[{"id":81675998,"asset_id":72964584,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":152571801,"first_name":"Andrea","last_name":"Buccino","domain_name":"independent","page_name":"AndreaBuccino","display_name":"Andrea Buccino","profile_url":"https://independent.academia.edu/AndreaBuccino?f_ri=334552","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=334552","nofollow":false},{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":46818,"name":"Exobiology","url":"https://www.academia.edu/Documents/in/Exobiology?f_ri=334552"},{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=334552"},{"id":112063,"name":"Uv Radiation","url":"https://www.academia.edu/Documents/in/Uv_Radiation?f_ri=334552"},{"id":137179,"name":"Origin of Life","url":"https://www.academia.edu/Documents/in/Origin_of_Life?f_ri=334552"},{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=334552"},{"id":220059,"name":"Subject headings","url":"https://www.academia.edu/Documents/in/Subject_headings?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":343860,"name":"Planetary system formation","url":"https://www.academia.edu/Documents/in/Planetary_system_formation?f_ri=334552"},{"id":351461,"name":"Biological systems","url":"https://www.academia.edu/Documents/in/Biological_systems?f_ri=334552"},{"id":517654,"name":"Icarus","url":"https://www.academia.edu/Documents/in/Icarus?f_ri=334552"},{"id":531200,"name":"Extraterrestrial Life","url":"https://www.academia.edu/Documents/in/Extraterrestrial_Life?f_ri=334552"},{"id":724456,"name":"Espectroscopía UV","url":"https://www.academia.edu/Documents/in/Espectroscopia_UV?f_ri=334552"},{"id":882081,"name":"Ultraviolet Radiation","url":"https://www.academia.edu/Documents/in/Ultraviolet_Radiation?f_ri=334552"},{"id":1003892,"name":"Energy Source","url":"https://www.academia.edu/Documents/in/Energy_Source?f_ri=334552"},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_42973999" data-work_id="42973999" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/42973999/The_First_Naked_Eye_Superflare_Detected_from_Proxima_Centauri">The First Naked-Eye Superflare Detected from Proxima Centauri</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Proxima b is a terrestrial-mass planet in the habitable-zone of Proxima Centauri. Proxima Centauri's high stellar activity however casts doubt on the habitability of Proxima b: sufficiently bright and frequent flares and any associated... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_42973999" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Proxima b is a terrestrial-mass planet in the habitable-zone of Proxima Centauri. Proxima Centauri's high stellar activity however casts doubt on the habitability of Proxima b: sufficiently bright and frequent flares and any associated proton events may destroy the planet's ozone layer, allowing lethal levels of UV flux to reach its surface. In March 2016, the Evryscope observed the first naked-eye-brightness superflare detected from Proxima Centauri. Proxima increased in optical flux by a factor of ~68 during the superflare and released a bolometric energy of 10^33.5 erg, ~10X larger than any previously-detected flare from Proxima. Over the last two years the Evryscope has recorded 23 other large Proxima flares ranging in bolometric energy from 10^30.6 erg to 10^32.4 erg; coupling those rates with the single superflare detection, we predict at least five superflares occur each year. Simultaneous high-resolution HARPS spectroscopy during the Evryscope superflare constrains the superflare's UV spectrum and any associated coronal mass ejections. We use these results and the Evryscope flare rates to model the photochemical effects of NOx atmospheric species generated by particle events from this extreme stellar activity, and show that the repeated flaring may be sufficient to reduce the ozone of an Earth-like atmosphere by 90% within five years; complete depletion may occur within several hundred kyr. The UV light produced by the Evryscope superflare would therefore have reached the surface with ~100X the intensity required to kill simple UV-hardy microorganisms, suggesting that life would have to undergo extreme adaptations to survive in the surface areas of Proxima b exposed to these flares.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/42973999" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="48f0a0bbc5afab3b42a5b6e1b2d5fec3" rel="nofollow" data-download="{"attachment_id":63232900,"asset_id":42973999,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/63232900/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="1388949" href="https://colorado.academia.edu/WardHoward">Ward Howard</a><script data-card-contents-for-user="1388949" type="text/json">{"id":1388949,"first_name":"Ward","last_name":"Howard","domain_name":"colorado","page_name":"WardHoward","display_name":"Ward Howard","profile_url":"https://colorado.academia.edu/WardHoward?f_ri=334552","photo":"https://0.academia-photos.com/1388949/11967649/104557713/s65_ward.howard.jpg"}</script></span></span></li><li class="js-paper-rank-work_42973999 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="42973999"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 42973999, container: ".js-paper-rank-work_42973999", }); });</script></li><li class="js-percentile-work_42973999 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 42973999; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_42973999"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_42973999 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="42973999"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 42973999; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=42973999]").text(description); $(".js-view-count-work_42973999").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_42973999").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="42973999"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">2</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="294031" href="https://www.academia.edu/Documents/in/Stellar_flares">Stellar flares</a>, <script data-card-contents-for-ri="294031" type="text/json">{"id":294031,"name":"Stellar flares","url":"https://www.academia.edu/Documents/in/Stellar_flares?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=42973999]'), work: {"id":42973999,"title":"The First Naked-Eye Superflare Detected from Proxima Centauri","created_at":"2020-05-07T15:01:56.225-07:00","url":"https://www.academia.edu/42973999/The_First_Naked_Eye_Superflare_Detected_from_Proxima_Centauri?f_ri=334552","dom_id":"work_42973999","summary":"Proxima b is a terrestrial-mass planet in the habitable-zone of Proxima Centauri. Proxima Centauri's high stellar activity however casts doubt on the habitability of Proxima b: sufficiently bright and frequent flares and any associated proton events may destroy the planet's ozone layer, allowing lethal levels of UV flux to reach its surface. In March 2016, the Evryscope observed the first naked-eye-brightness superflare detected from Proxima Centauri. Proxima increased in optical flux by a factor of ~68 during the superflare and released a bolometric energy of 10^33.5 erg, ~10X larger than any previously-detected flare from Proxima. Over the last two years the Evryscope has recorded 23 other large Proxima flares ranging in bolometric energy from 10^30.6 erg to 10^32.4 erg; coupling those rates with the single superflare detection, we predict at least five superflares occur each year. Simultaneous high-resolution HARPS spectroscopy during the Evryscope superflare constrains the superflare's UV spectrum and any associated coronal mass ejections. We use these results and the Evryscope flare rates to model the photochemical effects of NOx atmospheric species generated by particle events from this extreme stellar activity, and show that the repeated flaring may be sufficient to reduce the ozone of an Earth-like atmosphere by 90% within five years; complete depletion may occur within several hundred kyr. The UV light produced by the Evryscope superflare would therefore have reached the surface with ~100X the intensity required to kill simple UV-hardy microorganisms, suggesting that life would have to undergo extreme adaptations to survive in the surface areas of Proxima b exposed to these flares. ","downloadable_attachments":[{"id":63232900,"asset_id":42973999,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":1388949,"first_name":"Ward","last_name":"Howard","domain_name":"colorado","page_name":"WardHoward","display_name":"Ward Howard","profile_url":"https://colorado.academia.edu/WardHoward?f_ri=334552","photo":"https://0.academia-photos.com/1388949/11967649/104557713/s65_ward.howard.jpg"}],"research_interests":[{"id":294031,"name":"Stellar flares","url":"https://www.academia.edu/Documents/in/Stellar_flares?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_42973913 coauthored" data-work_id="42973913" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/42973913/EvryFlare_I_Long_term_Evryscope_Monitoring_of_Flares_from_the_Cool_Stars_Across_Half_the_Southern_Sky">EvryFlare I: Long-term Evryscope Monitoring of Flares from the Cool Stars Across Half the Southern Sky</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We search for superflares from 4,068 cool stars in 2+ years of Evryscope photometry, focusing on those with high-cadence data from both Evryscope and TESS. The Evryscope array of small telescopes observed 575 flares from 284 stars, with a... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_42973913" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We search for superflares from 4,068 cool stars in 2+ years of Evryscope photometry, focusing on those with high-cadence data from both Evryscope and TESS. The Evryscope array of small telescopes observed 575 flares from 284 stars, with a median energy of 10^34.0 erg. Since 2016, Evryscope has enabled the detection of rare events from all stars observed by TESS through multi-year, high-cadence continuous observing. We report ~2X the previous largest number of 10^34 erg high-cadence flares from nearby cool stars. We find 8 flares with amplitudes of 3+ g' magnitudes, with the largest reaching 5.6 magnitudes and releasing 10^36.2 erg. We observe a 10^34 erg superflare from TOI-455 (LTT 1445), a mid-M with a rocky planet candidate. We measure the superflare rate per flare-star and quantify the average flaring of active stars as a function of spectral type, including superflare rates, FFDs, and typical flare amplitudes in g'. We confirm superflare morphology is broadly consistent with magnetic re-connection. We estimate starspot coverage necessary to produce superflares, and hypothesize maximum-allowed superflare energies and waiting-times between flares corresponding to 100% coverage of the stellar hemisphere. We observe decreased flaring at high galactic latitudes. We explore the effects of superflares on ozone loss to planetary atmospheres: we observe 1 superflare with sufficient energy to photo-dissociate all ozone in an Earth-like atmosphere in one event. We find 17 stars that may deplete an Earth-like atmosphere via repeated flaring. Of the 1822 stars around which TESS may discover temperate rocky planets, we observe 14.6% +/- 2% emit large flares.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/42973913" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="a8f065174f29231276385d6058fd65e0" rel="nofollow" data-download="{"attachment_id":63232754,"asset_id":42973913,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/63232754/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="1388949" href="https://colorado.academia.edu/WardHoward">Ward Howard</a><script data-card-contents-for-user="1388949" type="text/json">{"id":1388949,"first_name":"Ward","last_name":"Howard","domain_name":"colorado","page_name":"WardHoward","display_name":"Ward Howard","profile_url":"https://colorado.academia.edu/WardHoward?f_ri=334552","photo":"https://0.academia-photos.com/1388949/11967649/104557713/s65_ward.howard.jpg"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-42973913">+1</span><div class="hidden js-additional-users-42973913"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://ub.academia.edu/OctaviFors">Octavi Fors</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-42973913'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-42973913').html(); 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container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_42973913 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="42973913"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 42973913; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=42973913]").text(description); $(".js-view-count-work_42973913").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_42973913").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="42973913"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">2</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="294031" href="https://www.academia.edu/Documents/in/Stellar_flares">Stellar flares</a>, <script data-card-contents-for-ri="294031" type="text/json">{"id":294031,"name":"Stellar flares","url":"https://www.academia.edu/Documents/in/Stellar_flares?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=42973913]'), work: {"id":42973913,"title":"EvryFlare I: Long-term Evryscope Monitoring of Flares from the Cool Stars Across Half the Southern Sky","created_at":"2020-05-07T14:47:08.782-07:00","url":"https://www.academia.edu/42973913/EvryFlare_I_Long_term_Evryscope_Monitoring_of_Flares_from_the_Cool_Stars_Across_Half_the_Southern_Sky?f_ri=334552","dom_id":"work_42973913","summary":"We search for superflares from 4,068 cool stars in 2+ years of Evryscope photometry, focusing on those with high-cadence data from both Evryscope and TESS. The Evryscope array of small telescopes observed 575 flares from 284 stars, with a median energy of 10^34.0 erg. Since 2016, Evryscope has enabled the detection of rare events from all stars observed by TESS through multi-year, high-cadence continuous observing. We report ~2X the previous largest number of 10^34 erg high-cadence flares from nearby cool stars. We find 8 flares with amplitudes of 3+ g' magnitudes, with the largest reaching 5.6 magnitudes and releasing 10^36.2 erg. We observe a 10^34 erg superflare from TOI-455 (LTT 1445), a mid-M with a rocky planet candidate. We measure the superflare rate per flare-star and quantify the average flaring of active stars as a function of spectral type, including superflare rates, FFDs, and typical flare amplitudes in g'. We confirm superflare morphology is broadly consistent with magnetic re-connection. We estimate starspot coverage necessary to produce superflares, and hypothesize maximum-allowed superflare energies and waiting-times between flares corresponding to 100% coverage of the stellar hemisphere. We observe decreased flaring at high galactic latitudes. We explore the effects of superflares on ozone loss to planetary atmospheres: we observe 1 superflare with sufficient energy to photo-dissociate all ozone in an Earth-like atmosphere in one event. We find 17 stars that may deplete an Earth-like atmosphere via repeated flaring. Of the 1822 stars around which TESS may discover temperate rocky planets, we observe 14.6% +/- 2% emit large flares. ","downloadable_attachments":[{"id":63232754,"asset_id":42973913,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":1388949,"first_name":"Ward","last_name":"Howard","domain_name":"colorado","page_name":"WardHoward","display_name":"Ward Howard","profile_url":"https://colorado.academia.edu/WardHoward?f_ri=334552","photo":"https://0.academia-photos.com/1388949/11967649/104557713/s65_ward.howard.jpg"},{"id":158193108,"first_name":"Octavi","last_name":"Fors","domain_name":"ub","page_name":"OctaviFors","display_name":"Octavi Fors","profile_url":"https://ub.academia.edu/OctaviFors?f_ri=334552","photo":"https://0.academia-photos.com/158193108/44284151/34913180/s65_octavi.fors.jpg"}],"research_interests":[{"id":294031,"name":"Stellar flares","url":"https://www.academia.edu/Documents/in/Stellar_flares?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_39791204" data-work_id="39791204" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/39791204/Apakah_Ada_Planet_Layak_Huni_Selain_Bumi">Apakah Ada Planet Layak Huni Selain Bumi?</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Di alam semesta ini ada banyak sekali benda-benda langit yang tidak jarang bisa kita lihat menggunakan mata telanjang. Tidak hanya komet atau Matahari, namun ada juga planet-planet yang menghiasi indahnya langit malam. Jika selama ini... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_39791204" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Di alam semesta ini ada banyak sekali benda-benda langit yang tidak jarang bisa kita lihat menggunakan mata telanjang. Tidak hanya komet atau Matahari, namun ada juga planet-planet yang menghiasi indahnya langit malam. Jika selama ini kita menyangka bahwa hanya ada Sembilan planet saja (termasuk Pluto), ternyata masih ada banyak planet-planet yang tidak kita ketahui, sehingga sejak abad ke 16, seorang filsuf dari Italia yang bernama Giordano Bruno mengemukakan pendapatnya mengenai "dunia lain."</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/39791204" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="abab72ac2e855131b08b0498c690b8f5" rel="nofollow" data-download="{"attachment_id":59977128,"asset_id":39791204,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/59977128/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="9997491" href="https://usu-id.academia.edu/BerthiannaNurcresia">Berthianna Nurcresia</a><script data-card-contents-for-user="9997491" type="text/json">{"id":9997491,"first_name":"Berthianna","last_name":"Nurcresia","domain_name":"usu-id","page_name":"BerthiannaNurcresia","display_name":"Berthianna Nurcresia","profile_url":"https://usu-id.academia.edu/BerthiannaNurcresia?f_ri=334552","photo":"https://0.academia-photos.com/9997491/3741791/38778696/s65_berthianna.nurcresia.jpg"}</script></span></span></li><li class="js-paper-rank-work_39791204 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="39791204"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 39791204, container: ".js-paper-rank-work_39791204", }); 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Tidak hanya komet atau Matahari, namun ada juga planet-planet yang menghiasi indahnya langit malam. Jika selama ini kita menyangka bahwa hanya ada Sembilan planet saja (termasuk Pluto), ternyata masih ada banyak planet-planet yang tidak kita ketahui, sehingga sejak abad ke 16, seorang filsuf dari Italia yang bernama Giordano Bruno mengemukakan pendapatnya mengenai \"dunia lain.\" ","downloadable_attachments":[{"id":59977128,"asset_id":39791204,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":9997491,"first_name":"Berthianna","last_name":"Nurcresia","domain_name":"usu-id","page_name":"BerthiannaNurcresia","display_name":"Berthianna Nurcresia","profile_url":"https://usu-id.academia.edu/BerthiannaNurcresia?f_ri=334552","photo":"https://0.academia-photos.com/9997491/3741791/38778696/s65_berthianna.nurcresia.jpg"}],"research_interests":[{"id":2417,"name":"Planetary Science","url":"https://www.academia.edu/Documents/in/Planetary_Science?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":675517,"name":"Physics and Astronomy","url":"https://www.academia.edu/Documents/in/Physics_and_Astronomy?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4200886" data-work_id="4200886" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4200886/The_Formation_of_Terrestrial_and_Giant_Exoplanets">The Formation of Terrestrial and Giant Exoplanets</a></div></div><div class="u-pb4x u-mt3x"></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4200886" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="18c767f8d9eaf0f0dc3748fd3c7c07fd" rel="nofollow" data-download="{"attachment_id":31695159,"asset_id":4200886,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31695159/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4200886 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4200886"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4200886, container: ".js-paper-rank-work_4200886", }); 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$(".js-view-count[data-work-id=4200886]").text(description); $(".js-view-count-work_4200886").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4200886").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4200886"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="6649" href="https://www.academia.edu/Documents/in/Infrared_Optics">Infrared Optics</a>, <script data-card-contents-for-ri="6649" type="text/json">{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="9820" href="https://www.academia.edu/Documents/in/Polarization_Ideology_">Polarization (Ideology)</a>, <script data-card-contents-for-ri="9820" type="text/json">{"id":9820,"name":"Polarization (Ideology)","url":"https://www.academia.edu/Documents/in/Polarization_Ideology_?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a><script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4200886]'), work: {"id":4200886,"title":"The Formation of Terrestrial and Giant Exoplanets","created_at":"2013-08-08T16:28:59.682-07:00","url":"https://www.academia.edu/4200886/The_Formation_of_Terrestrial_and_Giant_Exoplanets?f_ri=334552","dom_id":"work_4200886","summary":null,"downloadable_attachments":[{"id":31695159,"asset_id":4200886,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=334552","nofollow":false},{"id":9820,"name":"Polarization (Ideology)","url":"https://www.academia.edu/Documents/in/Polarization_Ideology_?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4156598" data-work_id="4156598" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4156598/The_effect_of_type_I_migration_on_the_formation_of_terrestrial_planets_in_hot_Jupiter_systems">The effect of type I migration on the formation of terrestrial planets in hot-Jupiter systems</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">"Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits, whilst scattering the rest into external... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4156598" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">"Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits, whilst scattering the rest into external orbits. Scattering tends to dominate, leaving behind abundant material that can accrete into terrestrial planets. <br />Aims. We add to the possible realism of our model by simulating type I migration forces which cause an inward drift, and strong eccentricity and inclination damping of protoplanetary bodies. This extra dissipation might be expected to enhance shepherding at the expense of scattering, possibly modifying our previous conclusions. <br />Methods. We employ an N-body code that is linked to a viscous gas disk algorithm capable of simulating: gas accretion onto the <br />central star; gap formation in the vicinity of the giant planet; type II migration of the giant planet; type I migration of protoplanets; and the effect of gas drag on planetesimals. We use the code to re-run three scenarios from a previous work where type I migration <br />was not included. <br />Results. The additional dissipation introduced by type I migration enhances the inward shepherding of material but does not severely reduce scattering. We find that >50% of the solids disk material still survives the migration in scattered exterior orbits: most of it well placed to complete terrestrial planet formation at <3 AU. The shepherded portion of the disk accretes into hot-Earths, which survive in interior orbits for the duration of our simulations. <br />Conclusions. Water-rich terrestrial planets can form in the habitable zones of hot-Jupiter systems and hot-Earths and hot-Neptunes may also be present. These systems should be targets of future planet search missions."</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4156598" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="efeadcd205e000db2b73aa665fbc0e4c" rel="nofollow" data-download="{"attachment_id":31663062,"asset_id":4156598,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31663062/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4156598 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4156598"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4156598, container: ".js-paper-rank-work_4156598", }); 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$(".js-view-count[data-work-id=4156598]").text(description); $(".js-view-count-work_4156598").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4156598").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4156598"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">9</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a><script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4156598]'), work: {"id":4156598,"title":"The effect of type I migration on the formation of terrestrial planets in hot-Jupiter systems","created_at":"2013-08-01T18:31:24.886-07:00","url":"https://www.academia.edu/4156598/The_effect_of_type_I_migration_on_the_formation_of_terrestrial_planets_in_hot_Jupiter_systems?f_ri=334552","dom_id":"work_4156598","summary":"\"Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits, whilst scattering the rest into external orbits. Scattering tends to dominate, leaving behind abundant material that can accrete into terrestrial planets.\r\nAims. We add to the possible realism of our model by simulating type I migration forces which cause an inward drift, and strong eccentricity and inclination damping of protoplanetary bodies. This extra dissipation might be expected to enhance shepherding at the expense of scattering, possibly modifying our previous conclusions.\r\nMethods. We employ an N-body code that is linked to a viscous gas disk algorithm capable of simulating: gas accretion onto the\r\ncentral star; gap formation in the vicinity of the giant planet; type II migration of the giant planet; type I migration of protoplanets; and the effect of gas drag on planetesimals. We use the code to re-run three scenarios from a previous work where type I migration\r\nwas not included.\r\nResults. The additional dissipation introduced by type I migration enhances the inward shepherding of material but does not severely reduce scattering. We find that \u003e50% of the solids disk material still survives the migration in scattered exterior orbits: most of it well placed to complete terrestrial planet formation at \u003c3 AU. The shepherded portion of the disk accretes into hot-Earths, which survive in interior orbits for the duration of our simulations.\r\nConclusions. Water-rich terrestrial planets can form in the habitable zones of hot-Jupiter systems and hot-Earths and hot-Neptunes may also be present. These systems should be targets of future planet search missions.\"","downloadable_attachments":[{"id":31663062,"asset_id":4156598,"asset_type":"Work","always_allow_download":false},{"id":31663027,"asset_id":4156598,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4156597" data-work_id="4156597" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4156597/Terrestrial_planet_formation_in_low_eccentricity_warm_Jupiter_systems">Terrestrial planet formation in low-eccentricity warm-Jupiter systems</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">""Context. Extrasolar giant planets are found to orbit their host stars with a broad range of semi-major axes 0.02 ≤ a ≤ 6 AU. Current theories suggest that giant planets orbiting at distances between 0.02−2 AU probably formed at larger... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4156597" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">""Context. Extrasolar giant planets are found to orbit their host stars with a broad range of semi-major axes 0.02 ≤ a ≤ 6 AU. Current theories suggest that giant planets orbiting at distances  between 0.02−2 AU probably formed at larger distances and  migrated to their current locations via type II migration, disturbing any inner system of forming terrestrial planets along the way. Migration probably halts because of fortuitously-timed gas disk dispersal. <br />Aims. The aim of this paper is to examine the effect of giant planet migration on the formation of inner terrestrial planet systems. We consider situations in which the giant planet halts migration at semi-major axes in the range 0.13−1.7 AU due to gas disk dispersal, and examine the effect of including or neglecting type I migration forces on the forming terrestrial system. <br />Methods. We employ an N-body code that is linked to a viscous gas disk algorithm capable of simulating gas loss via accretion onto the central star and photoevaporation, gap formation by the giant planet, type II migration of the giant, optional type I migration of protoplanets, and gas drag on planetesimals. <br />Results. Most of the inner system planetary building blocks survive the passage of the giant planet, either by being shepherded inward or scattered into exterior orbits. Systems of one or more hot-Earths are predicted to form and remain interior to the giant planet, especially if type II migration has been limited, or where type I migration has affected protoplanetary dynamics. Habitable planets in low-eccentricity warm-Jupiter systems appear possible if the giant planet makes a limited incursion into the outer regions of the habitable zone (HZ), or traverses its entire width and ceases migrating at a radial distance of less than half that of the HZ’s inner edge. <br />Conclusions. Type II migration does not prevent terrestrial planet formation. A wide variety of planetary system architectures exists that can potentially host habitable planets.""</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4156597" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="8da7e6c8322c37c73e71dae7243eb031" rel="nofollow" data-download="{"attachment_id":31663059,"asset_id":4156597,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31663059/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4156597 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4156597"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4156597, container: ".js-paper-rank-work_4156597", }); 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$(".js-view-count[data-work-id=4156597]").text(description); $(".js-view-count-work_4156597").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4156597").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4156597"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a><script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4156597]'), work: {"id":4156597,"title":"Terrestrial planet formation in low-eccentricity warm-Jupiter systems","created_at":"2013-08-01T18:31:24.558-07:00","url":"https://www.academia.edu/4156597/Terrestrial_planet_formation_in_low_eccentricity_warm_Jupiter_systems?f_ri=334552","dom_id":"work_4156597","summary":"\"\"Context. Extrasolar giant planets are found to orbit their host stars with a broad range of semi-major axes 0.02 ≤ a ≤ 6 AU. Current theories suggest that giant planets orbiting at distances between \u00040.02−2 AU probably formed at larger distances and migrated to their current locations via type II migration, disturbing any inner system of forming terrestrial planets along the way. Migration probably halts because of fortuitously-timed gas disk dispersal. \r\nAims. The aim of this paper is to examine the effect of giant planet migration on the formation of inner terrestrial planet systems. We consider situations in which the giant planet halts migration at semi-major axes in the range 0.13−1.7 AU due to gas disk dispersal, and examine the effect of including or neglecting type I migration forces on the forming terrestrial system.\r\nMethods. We employ an N-body code that is linked to a viscous gas disk algorithm capable of simulating gas loss via accretion onto the central star and photoevaporation, gap formation by the giant planet, type II migration of the giant, optional type I migration of protoplanets, and gas drag on planetesimals.\r\nResults. Most of the inner system planetary building blocks survive the passage of the giant planet, either by being shepherded inward or scattered into exterior orbits. Systems of one or more hot-Earths are predicted to form and remain interior to the giant planet, especially if type II migration has been limited, or where type I migration has affected protoplanetary dynamics. Habitable planets in low-eccentricity warm-Jupiter systems appear possible if the giant planet makes a limited incursion into the outer regions of the habitable zone (HZ), or traverses its entire width and ceases migrating at a radial distance of less than half that of the HZ’s inner edge.\r\nConclusions. Type II migration does not prevent terrestrial planet formation. A wide variety of planetary system architectures exists that can potentially host habitable planets.\"\"","downloadable_attachments":[{"id":31663059,"asset_id":4156597,"asset_type":"Work","always_allow_download":false},{"id":31663029,"asset_id":4156597,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4156598" data-work_id="4156598" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4156598/The_effect_of_type_I_migration_on_the_formation_of_terrestrial_planets_in_hot_Jupiter_systems">The effect of type I migration on the formation of terrestrial planets in hot-Jupiter systems</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">"Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits, whilst scattering the rest into external... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4156598" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">"Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits, whilst scattering the rest into external orbits. Scattering tends to dominate, leaving behind abundant material that can accrete into terrestrial planets. <br />Aims. We add to the possible realism of our model by simulating type I migration forces which cause an inward drift, and strong eccentricity and inclination damping of protoplanetary bodies. This extra dissipation might be expected to enhance shepherding at the expense of scattering, possibly modifying our previous conclusions. <br />Methods. We employ an N-body code that is linked to a viscous gas disk algorithm capable of simulating: gas accretion onto the <br />central star; gap formation in the vicinity of the giant planet; type II migration of the giant planet; type I migration of protoplanets; and the effect of gas drag on planetesimals. We use the code to re-run three scenarios from a previous work where type I migration <br />was not included. <br />Results. The additional dissipation introduced by type I migration enhances the inward shepherding of material but does not severely reduce scattering. We find that >50% of the solids disk material still survives the migration in scattered exterior orbits: most of it well placed to complete terrestrial planet formation at <3 AU. The shepherded portion of the disk accretes into hot-Earths, which survive in interior orbits for the duration of our simulations. <br />Conclusions. Water-rich terrestrial planets can form in the habitable zones of hot-Jupiter systems and hot-Earths and hot-Neptunes may also be present. These systems should be targets of future planet search missions."</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4156598" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="128ae87b9d33ff54e3144bb2f10cc96b" rel="nofollow" data-download="{"attachment_id":31663062,"asset_id":4156598,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31663062/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4156598 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4156598"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4156598, container: ".js-paper-rank-work_4156598", }); });</script></li><li class="js-percentile-work_4156598 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4156598; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4156598"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4156598 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4156598"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4156598; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4156598]").text(description); $(".js-view-count-work_4156598").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4156598").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4156598"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">9</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a><script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4156598]'), work: {"id":4156598,"title":"The effect of type I migration on the formation of terrestrial planets in hot-Jupiter systems","created_at":"2013-08-01T18:31:24.886-07:00","url":"https://www.academia.edu/4156598/The_effect_of_type_I_migration_on_the_formation_of_terrestrial_planets_in_hot_Jupiter_systems?f_ri=334552","dom_id":"work_4156598","summary":"\"Context. Our previous models of a giant planet migrating through an inner protoplanet/planetesimal disk find that the giant shepherds a portion of the material it encounters into interior orbits, whilst scattering the rest into external orbits. Scattering tends to dominate, leaving behind abundant material that can accrete into terrestrial planets.\r\nAims. We add to the possible realism of our model by simulating type I migration forces which cause an inward drift, and strong eccentricity and inclination damping of protoplanetary bodies. This extra dissipation might be expected to enhance shepherding at the expense of scattering, possibly modifying our previous conclusions.\r\nMethods. We employ an N-body code that is linked to a viscous gas disk algorithm capable of simulating: gas accretion onto the\r\ncentral star; gap formation in the vicinity of the giant planet; type II migration of the giant planet; type I migration of protoplanets; and the effect of gas drag on planetesimals. We use the code to re-run three scenarios from a previous work where type I migration\r\nwas not included.\r\nResults. The additional dissipation introduced by type I migration enhances the inward shepherding of material but does not severely reduce scattering. We find that \u003e50% of the solids disk material still survives the migration in scattered exterior orbits: most of it well placed to complete terrestrial planet formation at \u003c3 AU. The shepherded portion of the disk accretes into hot-Earths, which survive in interior orbits for the duration of our simulations.\r\nConclusions. Water-rich terrestrial planets can form in the habitable zones of hot-Jupiter systems and hot-Earths and hot-Neptunes may also be present. These systems should be targets of future planet search missions.\"","downloadable_attachments":[{"id":31663062,"asset_id":4156598,"asset_type":"Work","always_allow_download":false},{"id":31663027,"asset_id":4156598,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4156601" data-work_id="4156601" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4156601/On_the_possibility_of_terrestrial_planet_formation_in_hot_Jupiter_systems">On the possibility of terrestrial planet formation in hot-Jupiter systems</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">About a fifth of the exoplanetary systems that have been discovered contain a so-called hot-Jupiter – a giant planet orbiting within 0.1 AU of the central star. Since these stars are typically of the F/G spectral type, the orbits of any... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4156601" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">About a fifth of the exoplanetary systems that have been discovered contain a so-called hot-Jupiter – a giant planet orbiting within 0.1 AU of the central star. Since these stars are typically of the F/G spectral type, the orbits of any terrestrial planets in their habitable zones at y1 AU should be dynamically stable. However, because hot-Jupiters are thought to have formed in the outer regions of a protoplanetary disc, and to have then migrated through the terrestrial planet zone to their final location, it is uncertain whether terrestrial planets can actually grow and be retained in these systems. In this paper we review attempts to answer this question. Initial speculations, based on the assumption that migrating giant planets will clear planet-forming material from their swept zone, all concluded that hot-Jupiter systems should lack terrestrial planets. We show that this assumption may be incorrect, for when terrestrial planet formation and giant planet migration are simulated simultaneously, abundant solid material is predicted to remain from which terrestrial planet growth can resume.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4156601" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="b18307706341c12835eb1b7cf041bf5c" rel="nofollow" data-download="{"attachment_id":31663094,"asset_id":4156601,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31663094/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4156601 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4156601"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4156601, container: ".js-paper-rank-work_4156601", }); });</script></li><li class="js-percentile-work_4156601 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4156601; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4156601"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4156601 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4156601"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4156601; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4156601]").text(description); $(".js-view-count-work_4156601").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4156601").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4156601"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a><script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4156601]'), work: {"id":4156601,"title":"On the possibility of terrestrial planet formation in hot-Jupiter systems","created_at":"2013-08-01T18:31:25.621-07:00","url":"https://www.academia.edu/4156601/On_the_possibility_of_terrestrial_planet_formation_in_hot_Jupiter_systems?f_ri=334552","dom_id":"work_4156601","summary":"About a fifth of the exoplanetary systems that have been discovered contain a so-called hot-Jupiter – a giant planet orbiting within 0.1 AU of the central star. Since these stars are typically of the F/G spectral type, the orbits of any terrestrial planets in their habitable zones at y1 AU should be dynamically stable. However, because hot-Jupiters are thought to have formed in the outer regions of a protoplanetary disc, and to have then migrated through the terrestrial planet zone to their final location, it is uncertain whether terrestrial planets can actually grow and be retained in these systems. In this paper we review attempts to answer this question. Initial speculations, based on the assumption that migrating giant planets will clear planet-forming material from their swept zone, all concluded that hot-Jupiter systems should lack terrestrial planets. We show that this assumption may be incorrect, for when terrestrial planet formation and giant planet migration are simulated simultaneously, abundant solid material is predicted to remain from which terrestrial planet growth can resume.","downloadable_attachments":[{"id":31663094,"asset_id":4156601,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_75642534" data-work_id="75642534" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/75642534/Wind_driven_Western_Boundary_Ocean_Currents_in_Terran_and_Superterran_Exoplanets">Wind-driven Western Boundary Ocean Currents in Terran and Superterran Exoplanets</a></div></div><div class="u-pb4x u-mt3x"></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/75642534" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="6514171" href="https://uprm.academia.edu/EdwinAlfonsoSosa">Edwin Alfonso-Sosa</a><script data-card-contents-for-user="6514171" type="text/json">{"id":6514171,"first_name":"Edwin","last_name":"Alfonso-Sosa","domain_name":"uprm","page_name":"EdwinAlfonsoSosa","display_name":"Edwin Alfonso-Sosa","profile_url":"https://uprm.academia.edu/EdwinAlfonsoSosa?f_ri=334552","photo":"https://0.academia-photos.com/6514171/2620257/15741845/s65_edwin.alfonso-sosa.jpg"}</script></span></span></li><li class="js-paper-rank-work_75642534 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" 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data-work-id="4200867"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4200867; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4200867]").text(description); $(".js-view-count-work_4200867").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4200867").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4200867"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">10</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="4363" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="6649" href="https://www.academia.edu/Documents/in/Infrared_Optics">Infrared Optics</a>, <script data-card-contents-for-ri="6649" type="text/json">{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="9820" href="https://www.academia.edu/Documents/in/Polarization_Ideology_">Polarization (Ideology)</a><script data-card-contents-for-ri="9820" type="text/json">{"id":9820,"name":"Polarization (Ideology)","url":"https://www.academia.edu/Documents/in/Polarization_Ideology_?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4200867]'), work: {"id":4200867,"title":"The Formation of Terrestrial Planets in Hot Jupiter Systems,","created_at":"2013-08-08T16:23:19.330-07:00","url":"https://www.academia.edu/4200867/The_Formation_of_Terrestrial_Planets_in_Hot_Jupiter_Systems_?f_ri=334552","dom_id":"work_4200867","summary":null,"downloadable_attachments":[{"id":31695133,"asset_id":4200867,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=334552","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=334552","nofollow":false},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=334552","nofollow":false},{"id":9820,"name":"Polarization (Ideology)","url":"https://www.academia.edu/Documents/in/Polarization_Ideology_?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552"},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=334552"},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=334552"},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_44358423" data-work_id="44358423" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/44358423/Ultraviolet_radiation_constraints_around_the_circumstellar_habitable_zones">Ultraviolet radiation constraints around the circumstellar habitable zones</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between 200 and 300 nm becomes energetically very damaging to most of... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_44358423" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In<br />particular, UV radiation between 200 and 300 nm becomes energetically very damaging to most of the terrestrial biological systems. On the other<br />hand, UV radiation is usually considered one of the most important energy source on the primitive Earth for the synthesis of many biochemical compounds and, therefore, essential for several biogenesis processes. In this work, we use these properties of the UV radiation to define the boundaries of an ultraviolet habitable zone. We also analyze the evolution of the UV habitable zone during the main sequence stage of the star. We apply these criteria to study the UV habitable zone for those extrasolar planetary systems that were observed by the International Ultraviolet Explorer (IUE). We analyze the possibility that extrasolar planets and moons could be suitable for life, according to the UV constrains presented in this work and other accepted criteria of habitability (liquid water, orbital stability, etc.).</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/44358423" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="569750a6bc8f3ce29f61bc3082471d18" rel="nofollow" data-download="{"attachment_id":64753736,"asset_id":44358423,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/64753736/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="31221696" href="https://ajitha.academia.edu/GuillermoLemarchand">Guillermo A . Lemarchand</a><script data-card-contents-for-user="31221696" type="text/json">{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . 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In\nparticular, UV radiation between 200 and 300 nm becomes energetically very damaging to most of the terrestrial biological systems. On the other\nhand, UV radiation is usually considered one of the most important energy source on the primitive Earth for the synthesis of many biochemical compounds and, therefore, essential for several biogenesis processes. In this work, we use these properties of the UV radiation to define the boundaries of an ultraviolet habitable zone. We also analyze the evolution of the UV habitable zone during the main sequence stage of the star. We apply these criteria to study the UV habitable zone for those extrasolar planetary systems that were observed by the International Ultraviolet Explorer (IUE). We analyze the possibility that extrasolar planets and moons could be suitable for life, according to the UV constrains presented in this work and other accepted criteria of habitability (liquid water, orbital stability, etc.).","downloadable_attachments":[{"id":64753736,"asset_id":44358423,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":31221696,"first_name":"Guillermo","last_name":"Lemarchand","domain_name":"ajitha","page_name":"GuillermoLemarchand","display_name":"Guillermo A . Lemarchand","profile_url":"https://ajitha.academia.edu/GuillermoLemarchand?f_ri=334552","photo":"https://0.academia-photos.com/31221696/56593562/44799447/s65_guillermo.lemarchand.jpg"}],"research_interests":[{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":36271,"name":"SETI (Search for Extraterrestrial Intelligence)","url":"https://www.academia.edu/Documents/in/SETI_Search_for_Extraterrestrial_Intelligence_?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":531200,"name":"Extraterrestrial Life","url":"https://www.academia.edu/Documents/in/Extraterrestrial_Life?f_ri=334552"},{"id":724456,"name":"Espectroscopía UV","url":"https://www.academia.edu/Documents/in/Espectroscopia_UV?f_ri=334552"},{"id":791527,"name":"Bioastronomy \u0026 Exobiology","url":"https://www.academia.edu/Documents/in/Bioastronomy_and_Exobiology?f_ri=334552"},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_15328303" data-work_id="15328303" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/15328303/ERRATUM_HABITABLE_ZONES_AROUND_MAIN_SEQUENCE_STARS_NEW_ESTIMATES_2013_ApJ_765_131_">ERRATUM:“HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES”(2013, ApJ, 765, 131)</a></div></div><div class="u-pb4x u-mt3x"></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/15328303" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="0a9d2165a5c3493f1feef6f6355cb5b7" rel="nofollow" data-download="{"attachment_id":43331367,"asset_id":15328303,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/43331367/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="34439997" href="https://independent.academia.edu/ShawnDomagalgoldman">Shawn Domagal-goldman</a><script data-card-contents-for-user="34439997" type="text/json">{"id":34439997,"first_name":"Shawn","last_name":"Domagal-goldman","domain_name":"independent","page_name":"ShawnDomagalgoldman","display_name":"Shawn Domagal-goldman","profile_url":"https://independent.academia.edu/ShawnDomagalgoldman?f_ri=334552","photo":"https://0.academia-photos.com/34439997/10075327/11240322/s65_shawn.domagal-goldman.jpg"}</script></span></span></li><li class="js-paper-rank-work_15328303 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="15328303"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 15328303, container: ".js-paper-rank-work_15328303", }); 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$(".js-view-count[data-work-id=15328303]").text(description); $(".js-view-count-work_15328303").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_15328303").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="15328303"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">7</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="531" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="723" href="https://www.academia.edu/Documents/in/Astrophysical_Plasma">Astrophysical Plasma</a>, <script data-card-contents-for-ri="723" type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="138103" href="https://www.academia.edu/Documents/in/Aliens">Aliens</a><script data-card-contents-for-ri="138103" type="text/json">{"id":138103,"name":"Aliens","url":"https://www.academia.edu/Documents/in/Aliens?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=15328303]'), work: {"id":15328303,"title":"ERRATUM:“HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES”(2013, ApJ, 765, 131)","created_at":"2015-09-01T10:35:32.506-07:00","url":"https://www.academia.edu/15328303/ERRATUM_HABITABLE_ZONES_AROUND_MAIN_SEQUENCE_STARS_NEW_ESTIMATES_2013_ApJ_765_131_?f_ri=334552","dom_id":"work_15328303","summary":null,"downloadable_attachments":[{"id":43331367,"asset_id":15328303,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":34439997,"first_name":"Shawn","last_name":"Domagal-goldman","domain_name":"independent","page_name":"ShawnDomagalgoldman","display_name":"Shawn Domagal-goldman","profile_url":"https://independent.academia.edu/ShawnDomagalgoldman?f_ri=334552","photo":"https://0.academia-photos.com/34439997/10075327/11240322/s65_shawn.domagal-goldman.jpg"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=334552","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":138103,"name":"Aliens","url":"https://www.academia.edu/Documents/in/Aliens?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552"},{"id":406486,"name":"Habitability","url":"https://www.academia.edu/Documents/in/Habitability?f_ri=334552"},{"id":1336364,"name":"Habitable Zones","url":"https://www.academia.edu/Documents/in/Habitable_Zones?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_8604664" data-work_id="8604664" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/8604664/Geothermal_heating_enhances_atmospheric_asymmetries_on_synchronously_rotating_planets"> Geothermal heating enhances atmospheric asymmetries on synchronously rotating planets</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Earth-like planets within the liquid water habitable zone of M type stars may evolve into synchronous rotators. On these planets, the sub-stellar hemisphere experiences perpetual daylight while the opposing anti-stellar hemisphere... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_8604664" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Earth-like planets within the liquid water habitable zone of M type stars may evolve into synchronous rotators. On these planets, the sub-stellar hemisphere experiences perpetual daylight while the opposing anti-stellar hemisphere experiences perpetual darkness. Because the night-side hemisphere has no direct source of energy, the air over this side of the planet is prone to freeze out and deposit on the surface, which could result in atmospheric collapse. However, general circulation models (GCMs) have shown that atmospheric dynamics can counteract this problem and provide sufficient energy transport to the anti-stellar side.<br />Here we use an idealized GCM to consider the impact of geothermal heating on the habitability of synchronously rotating planets. Geothermal heating may be expected due to tidal interactions with the host star, and the effects of geothermal heating provide additional habitable surface area and may help to induce melting of ice on the anti-stellar hemisphere. We also explore the persistence of atmospheric asymmetries between the northern and southern hemispheres, and we find that the direction of the meridional circulation (for rapidly rotating planets) or the direction of zonal wind (for slowly rotating planets) reverses on either side of the sub-stellar point. We show that the zonal circulation approaches a theoretical state similar to a Walker circulation only for slowly rotating planets, while rapidly rotating planets show a zonal circulation with the opposite direction. We find that a cross-polar circulation is present in all cases and provides an additional mechanism of mass and energy transport from the sub-stellar to anti-stellar point. Characterization of the atmospheres of synchronously rotating planets should include consideration of hemispheric differences in meridional circulation and examination of transport due to cross-polar flow.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/8604664" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="2de079c426d0100846b802741119545f" rel="nofollow" data-download="{"attachment_id":34970804,"asset_id":8604664,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/34970804/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="3494" href="https://geosc-psu.academia.edu/RaviKopparapu">Ravi Kopparapu</a><script data-card-contents-for-user="3494" type="text/json">{"id":3494,"first_name":"Ravi","last_name":"Kopparapu","domain_name":"geosc-psu","page_name":"RaviKopparapu","display_name":"Ravi Kopparapu","profile_url":"https://geosc-psu.academia.edu/RaviKopparapu?f_ri=334552","photo":"https://0.academia-photos.com/3494/1191320/4773211/s65_ravi.kopparapu.png"}</script></span></span></li><li class="js-paper-rank-work_8604664 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="8604664"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 8604664, container: ".js-paper-rank-work_8604664", }); 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$(".js-view-count[data-work-id=8604664]").text(description); $(".js-view-count-work_8604664").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_8604664").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="8604664"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="30959" href="https://www.academia.edu/Documents/in/Climate_modeling">Climate modeling</a>, <script data-card-contents-for-ri="30959" type="text/json">{"id":30959,"name":"Climate modeling","url":"https://www.academia.edu/Documents/in/Climate_modeling?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="41236" href="https://www.academia.edu/Documents/in/Extrasolar_planets">Extrasolar planets</a>, <script data-card-contents-for-ri="41236" type="text/json">{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="161675" href="https://www.academia.edu/Documents/in/Three_dimensional_modeling_and_simulation">Three dimensional modeling and simulation</a>, <script data-card-contents-for-ri="161675" type="text/json">{"id":161675,"name":"Three dimensional modeling and simulation","url":"https://www.academia.edu/Documents/in/Three_dimensional_modeling_and_simulation?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=8604664]'), work: {"id":8604664,"title":" Geothermal heating enhances atmospheric asymmetries on synchronously rotating planets","created_at":"2014-10-02T05:38:03.673-07:00","url":"https://www.academia.edu/8604664/Geothermal_heating_enhances_atmospheric_asymmetries_on_synchronously_rotating_planets?f_ri=334552","dom_id":"work_8604664","summary":"Earth-like planets within the liquid water habitable zone of M type stars may evolve into synchronous rotators. On these planets, the sub-stellar hemisphere experiences perpetual daylight while the opposing anti-stellar hemisphere experiences perpetual darkness. Because the night-side hemisphere has no direct source of energy, the air over this side of the planet is prone to freeze out and deposit on the surface, which could result in atmospheric collapse. However, general circulation models (GCMs) have shown that atmospheric dynamics can counteract this problem and provide sufficient energy transport to the anti-stellar side.\nHere we use an idealized GCM to consider the impact of geothermal heating on the habitability of synchronously rotating planets. Geothermal heating may be expected due to tidal interactions with the host star, and the effects of geothermal heating provide additional habitable surface area and may help to induce melting of ice on the anti-stellar hemisphere. We also explore the persistence of atmospheric asymmetries between the northern and southern hemispheres, and we find that the direction of the meridional circulation (for rapidly rotating planets) or the direction of zonal wind (for slowly rotating planets) reverses on either side of the sub-stellar point. We show that the zonal circulation approaches a theoretical state similar to a Walker circulation only for slowly rotating planets, while rapidly rotating planets show a zonal circulation with the opposite direction. We find that a cross-polar circulation is present in all cases and provides an additional mechanism of mass and energy transport from the sub-stellar to anti-stellar point. Characterization of the atmospheres of synchronously rotating planets should include consideration of hemispheric differences in meridional circulation and examination of transport due to cross-polar flow. ","downloadable_attachments":[{"id":34970804,"asset_id":8604664,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":3494,"first_name":"Ravi","last_name":"Kopparapu","domain_name":"geosc-psu","page_name":"RaviKopparapu","display_name":"Ravi Kopparapu","profile_url":"https://geosc-psu.academia.edu/RaviKopparapu?f_ri=334552","photo":"https://0.academia-photos.com/3494/1191320/4773211/s65_ravi.kopparapu.png"}],"research_interests":[{"id":30959,"name":"Climate modeling","url":"https://www.academia.edu/Documents/in/Climate_modeling?f_ri=334552","nofollow":false},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=334552","nofollow":false},{"id":161675,"name":"Three dimensional modeling and simulation","url":"https://www.academia.edu/Documents/in/Three_dimensional_modeling_and_simulation?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false},{"id":1525381,"name":"Red Dwarf Stars,","url":"https://www.academia.edu/Documents/in/Red_Dwarf_Stars_?f_ri=334552"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_49080578 coauthored" data-work_id="49080578" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/49080578/Limitations_of_TESS_in_characterizing_the_first_habitable_zone_Earth_sized_planet">Limitations of TESS in characterizing the first habitable zone Earth-sized planet</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Recently, the TOI-700 System was characterized as the first habitable-zone Earth-sized planet using Transiting Exoplanet Survey Satellite (TESS). Ground-based follow-up combined with diagnostic vetting and validation tests enables this... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_49080578" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Recently, the TOI-700 System was characterized as the first habitable-zone Earth-sized planet using Transiting Exoplanet Survey Satellite (TESS). Ground-based follow-up combined with diagnostic vetting and validation tests enables this system to rule out common astrophysical false-positive scenarios and validate the planetary data.  However, TESS systems are restricted by a Nyquist limit that can interfere with internal structure data, especially at different oscillation modes. Another key limitation is the necessity of an ultra-stable light source for standardization purposes. Although several studies have shown promise, reliable data has yet to be validated.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/49080578" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="181249304" href="https://independent.academia.edu/JohnChristyJohnson">John Christy Johnson</a><script data-card-contents-for-user="181249304" type="text/json">{"id":181249304,"first_name":"John Christy","last_name":"Johnson","domain_name":"independent","page_name":"JohnChristyJohnson","display_name":"John Christy Johnson","profile_url":"https://independent.academia.edu/JohnChristyJohnson?f_ri=334552","photo":"https://0.academia-photos.com/181249304/51847700/39937750/s65_john_christy.johnson.jpg"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-49080578">+2</span><div class="hidden js-additional-users-49080578"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/PeterJohnson96">Peter A Johnson</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://ualberta.academia.edu/AustinMardon">Austin A Mardon</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-49080578'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-49080578').html(); } } new HoverPopover(popoverSettings); })();</script></li><li class="js-paper-rank-work_49080578 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="49080578"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 49080578, container: ".js-paper-rank-work_49080578", }); });</script></li><li class="js-percentile-work_49080578 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 49080578; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_49080578"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_49080578 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="49080578"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 49080578; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=49080578]").text(description); $(".js-view-count-work_49080578").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_49080578").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="49080578"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">3</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="5765" href="https://www.academia.edu/Documents/in/Satellite_Technology">Satellite Technology</a>, <script data-card-contents-for-ri="5765" type="text/json">{"id":5765,"name":"Satellite Technology","url":"https://www.academia.edu/Documents/in/Satellite_Technology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=49080578]'), work: {"id":49080578,"title":"Limitations of TESS in characterizing the first habitable zone Earth-sized planet","created_at":"2021-05-31T09:32:31.344-07:00","url":"https://www.academia.edu/49080578/Limitations_of_TESS_in_characterizing_the_first_habitable_zone_Earth_sized_planet?f_ri=334552","dom_id":"work_49080578","summary":"Recently, the TOI-700 System was characterized as the first habitable-zone Earth-sized planet using Transiting Exoplanet Survey Satellite (TESS). Ground-based follow-up combined with diagnostic vetting and validation tests enables this system to rule out common astrophysical false-positive scenarios and validate the planetary data. However, TESS systems are restricted by a Nyquist limit that can interfere with internal structure data, especially at different oscillation modes. Another key limitation is the necessity of an ultra-stable light source for standardization purposes. Although several studies have shown promise, reliable data has yet to be validated.","downloadable_attachments":[],"ordered_authors":[{"id":181249304,"first_name":"John Christy","last_name":"Johnson","domain_name":"independent","page_name":"JohnChristyJohnson","display_name":"John Christy Johnson","profile_url":"https://independent.academia.edu/JohnChristyJohnson?f_ri=334552","photo":"https://0.academia-photos.com/181249304/51847700/39937750/s65_john_christy.johnson.jpg"},{"id":32940668,"first_name":"Peter","last_name":"Johnson","domain_name":"independent","page_name":"PeterJohnson96","display_name":"Peter A Johnson","profile_url":"https://independent.academia.edu/PeterJohnson96?f_ri=334552","photo":"https://0.academia-photos.com/32940668/27255425/42461692/s65_peter.johnson.jpg"},{"id":5401149,"first_name":"Austin","last_name":"Mardon","domain_name":"ualberta","page_name":"AustinMardon","display_name":"Austin A Mardon","profile_url":"https://ualberta.academia.edu/AustinMardon?f_ri=334552","photo":"https://0.academia-photos.com/5401149/2371340/2762654/s65_austin.mardon.jpg"}],"research_interests":[{"id":5765,"name":"Satellite Technology","url":"https://www.academia.edu/Documents/in/Satellite_Technology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_43510855" data-work_id="43510855" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/43510855/Astrobiology_Research_6_">Astrobiology Research (6)</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">P1 Habitability The current habitability potential analysis of p1 has been acquired through the specifications that were calculated and provided for this project. We will dive in detail through the planet's physical and orbital data... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_43510855" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">P1 Habitability The current habitability potential analysis of p1 has been acquired through the specifications that were calculated and provided for this project. We will dive in detail through the planet's physical and orbital data including the stellar and system properties of the hosting planet. From looking at initial data, we can see that p1 is orbiting a close binary system where the two stars have a small enough distance allowing the gravitational attraction from each star forming an orbit between the stars around a barycenter. These stellar systems do have a habitable zone where liquid water could exist on the planet existing in these boundaries, however, similar to previous research shown on Kepler 47c, these planets are not guaranteed to have a stable foothold in the stellar goldilocks zone and might sometimes position out of zone boundaries during their orbits. This makes potential for life more difficult due to extreme changes of temperature and weather on the planet, occasionally freezing or warming up beyond limits of life. However as research suggests, an estimate of 50-60% of binary systems are capable of holding habitable terrestrial planets within their stable orbital range. 1 The planets in these systems have an S-type or P-type orbit in relation to their host stars. S-type is when orbit is within relation to one of the stars and P-type is in relation to both stellar objects. In order for p1 to have a high chance of habitability, it should have a stable orbit where p-type orbital properties are met with the right distance and inclination towards their stellar host, where the distance from the planet to the star is significantly larger than the star-star orbital distance. Since we know this is the case for p1 from the parameters given. We can move on to star types. The type of stars in p1 system are of spectral class A and K stars, for a star to be suitable for sustaining habitable planet, it should meet a certain criteria; it should have a high variety of elemental proportion not considering hydrogen and helium, in order to allow for the planet formation, since we already examining a planet, the compositions should probably be in check, next we need a star with mass small enough to allow longer lifetime, this is so life has a chance to take place on the stars habitable worlds, A class stars are white coloured stars with temperatures ranging from 7500K to 10000K, With a large mass and high luminosity factors, they have a much shorter life spans compared to smaller stars such as G,K and M spectral classes, at an estimate of 1 billion years for its main sequence life span. Knowing that the earliest evidence of life on earth is around 3.5 billion years old and that our solar system is 4.571 billion years old. We can say that an estimate of 1 billion years of right stellar-planetary conditions must exist for the planet to harbour habitability, at least according to the earth's model. This means that a short life span of A class stars make them not suitable for long term condition hospitality that allows for life, However, With a long orbital period of 6.38 years and the planet's semi major axis being at 4.66 AU, the distance of the planet from the binary system is significant enough where hospitable conditions might sustain life, Although, with the intense luminosity factor of 9.84 units from the Star A, intense radiation might make it difficult for planet to offer hospitality. Since the system is around 1.75 billion years old, Star A should have exhausted its age for its main sequence. Meaning that at the current stage it should be cooling down into a red giant. Unless the data is showing that currently the star is A type. The other star in the system being a K type in spectral class. It is a much cooler orange star with luminosity factor of 0.269 stellar units and stellar radius of 0.733, making it a much calmer star, within the category that have planets with high potential of harbouring life. These stars have a much longer life span nearing 50 billion years as estimated, giving suitable conditions for life within plants of its habitable zone for a significant amount of time. Considering that the p1 has a p-type orbit around these stars with a stable orbit far from these stars. It is difficult to believe that with intense alterations in luminosity</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/43510855" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="01f9d46179eae5ad75d09046bd17aabb" rel="nofollow" data-download="{"attachment_id":63821419,"asset_id":43510855,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/63821419/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="20708106" href="https://utoronto.academia.edu/ArvinSh">Arvin Sh</a><script data-card-contents-for-user="20708106" type="text/json">{"id":20708106,"first_name":"Arvin","last_name":"Sh","domain_name":"utoronto","page_name":"ArvinSh","display_name":"Arvin Sh","profile_url":"https://utoronto.academia.edu/ArvinSh?f_ri=334552","photo":"https://0.academia-photos.com/20708106/5731175/117214767/s65_arvin.sh.png"}</script></span></span></li><li class="js-paper-rank-work_43510855 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="43510855"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 43510855, container: ".js-paper-rank-work_43510855", }); });</script></li><li class="js-percentile-work_43510855 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 43510855; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_43510855"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_43510855 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="43510855"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 43510855; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=43510855]").text(description); $(".js-view-count-work_43510855").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_43510855").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="43510855"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">3</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="5001" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11056" href="https://www.academia.edu/Documents/in/Exoplanets">Exoplanets</a>, <script data-card-contents-for-ri="11056" type="text/json">{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=43510855]'), work: {"id":43510855,"title":"Astrobiology Research (6)","created_at":"2020-07-03T13:35:19.684-07:00","url":"https://www.academia.edu/43510855/Astrobiology_Research_6_?f_ri=334552","dom_id":"work_43510855","summary":" P1 Habitability The current habitability potential analysis of p1 has been acquired through the specifications that were calculated and provided for this project. We will dive in detail through the planet's physical and orbital data including the stellar and system properties of the hosting planet. From looking at initial data, we can see that p1 is orbiting a close binary system where the two stars have a small enough distance allowing the gravitational attraction from each star forming an orbit between the stars around a barycenter. These stellar systems do have a habitable zone where liquid water could exist on the planet existing in these boundaries, however, similar to previous research shown on Kepler 47c, these planets are not guaranteed to have a stable foothold in the stellar goldilocks zone and might sometimes position out of zone boundaries during their orbits. This makes potential for life more difficult due to extreme changes of temperature and weather on the planet, occasionally freezing or warming up beyond limits of life. However as research suggests, an estimate of 50-60% of binary systems are capable of holding habitable terrestrial planets within their stable orbital range. 1 The planets in these systems have an S-type or P-type orbit in relation to their host stars. S-type is when orbit is within relation to one of the stars and P-type is in relation to both stellar objects. In order for p1 to have a high chance of habitability, it should have a stable orbit where p-type orbital properties are met with the right distance and inclination towards their stellar host, where the distance from the planet to the star is significantly larger than the star-star orbital distance. Since we know this is the case for p1 from the parameters given. We can move on to star types. The type of stars in p1 system are of spectral class A and K stars, for a star to be suitable for sustaining habitable planet, it should meet a certain criteria; it should have a high variety of elemental proportion not considering hydrogen and helium, in order to allow for the planet formation, since we already examining a planet, the compositions should probably be in check, next we need a star with mass small enough to allow longer lifetime, this is so life has a chance to take place on the stars habitable worlds, A class stars are white coloured stars with temperatures ranging from 7500K to 10000K, With a large mass and high luminosity factors, they have a much shorter life spans compared to smaller stars such as G,K and M spectral classes, at an estimate of 1 billion years for its main sequence life span. Knowing that the earliest evidence of life on earth is around 3.5 billion years old and that our solar system is 4.571 billion years old. We can say that an estimate of 1 billion years of right stellar-planetary conditions must exist for the planet to harbour habitability, at least according to the earth's model. This means that a short life span of A class stars make them not suitable for long term condition hospitality that allows for life, However, With a long orbital period of 6.38 years and the planet's semi major axis being at 4.66 AU, the distance of the planet from the binary system is significant enough where hospitable conditions might sustain life, Although, with the intense luminosity factor of 9.84 units from the Star A, intense radiation might make it difficult for planet to offer hospitality. Since the system is around 1.75 billion years old, Star A should have exhausted its age for its main sequence. Meaning that at the current stage it should be cooling down into a red giant. Unless the data is showing that currently the star is A type. The other star in the system being a K type in spectral class. It is a much cooler orange star with luminosity factor of 0.269 stellar units and stellar radius of 0.733, making it a much calmer star, within the category that have planets with high potential of harbouring life. These stars have a much longer life span nearing 50 billion years as estimated, giving suitable conditions for life within plants of its habitable zone for a significant amount of time. Considering that the p1 has a p-type orbit around these stars with a stable orbit far from these stars. It is difficult to believe that with intense alterations in luminosity","downloadable_attachments":[{"id":63821419,"asset_id":43510855,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":20708106,"first_name":"Arvin","last_name":"Sh","domain_name":"utoronto","page_name":"ArvinSh","display_name":"Arvin Sh","profile_url":"https://utoronto.academia.edu/ArvinSh?f_ri=334552","photo":"https://0.academia-photos.com/20708106/5731175/117214767/s65_arvin.sh.png"}],"research_interests":[{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=334552","nofollow":false},{"id":11056,"name":"Exoplanets","url":"https://www.academia.edu/Documents/in/Exoplanets?f_ri=334552","nofollow":false},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=334552","nofollow":false}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_42681250" data-work_id="42681250" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/42681250/How_Metallicity_Affects_Volatile_Abundances_Implications_for_Planetary_System_Formation">How Metallicity Affects Volatile Abundances: Implications for Planetary System Formation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Astronomers have confirmed the existence of several thousand extra-solar planetary systems having a wide range of orbital and compositional characteristics. A host star's metallicity, defined as the abundance of all elements heavier than... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_42681250" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Astronomers have confirmed the existence of several thousand extra-solar planetary systems having a wide range of orbital and compositional characteristics. A host star's metallicity, defined as the abundance of all elements heavier than helium (metals), appears to play a role in determining whether an exoplanetary system is more likely to include Jupiter-sized gas and ice giants. Here we show how molecular cloud metallicity is likely to significantly affect the initial conditions of planetary formation by affecting the abundances of volatile ices (H 2 O, CO, etc.) in parent molecular clouds. Through analytic and numerical treatments of molecular chemical lifetimes, we show that volatile elements are more likely to be found as ices in metal rich clouds compared to metal poor ones. These correlations, in turn, may impact the characteristics of planetary systems as a function of their metallicity as suggested by the systematic shifts in snowline distances as a function of metallicity. We evaluate the "wet Earth" hypothesis for the origins of Earth's water and find that elevated protoplanetary disk pressures are required to retain the required partial (∼ 2%) monolayer of water on interstellar dust grain surfaces with MRN distribution.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/42681250" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="773b9d54767bfeb4d10cd86f28b7edeb" rel="nofollow" data-download="{"attachment_id":62890524,"asset_id":42681250,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/62890524/download_file?st=MTczMjM5NTQ0MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="28372593" href="https://independent.academia.edu/GerardoDominguez8">Gerardo Dominguez</a><script data-card-contents-for-user="28372593" type="text/json">{"id":28372593,"first_name":"Gerardo","last_name":"Dominguez","domain_name":"independent","page_name":"GerardoDominguez8","display_name":"Gerardo Dominguez","profile_url":"https://independent.academia.edu/GerardoDominguez8?f_ri=334552","photo":"https://0.academia-photos.com/28372593/8015565/8977505/s65_gerardo.dominguez.jpg"}</script></span></span></li><li class="js-paper-rank-work_42681250 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="42681250"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 42681250, container: ".js-paper-rank-work_42681250", }); 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We evaluate the \"wet Earth\" hypothesis for the origins of Earth's water and find that elevated protoplanetary disk pressures are required to retain the required partial (∼ 2%) monolayer of water on interstellar dust grain surfaces with MRN distribution.","downloadable_attachments":[{"id":62890524,"asset_id":42681250,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":28372593,"first_name":"Gerardo","last_name":"Dominguez","domain_name":"independent","page_name":"GerardoDominguez8","display_name":"Gerardo Dominguez","profile_url":"https://independent.academia.edu/GerardoDominguez8?f_ri=334552","photo":"https://0.academia-photos.com/28372593/8015565/8977505/s65_gerardo.dominguez.jpg"}],"research_interests":[{"id":716,"name":"Interstellar 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