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star</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 Faint Object Spectrograph (FOS) aboard Hubble Space Telescope (HST) has been used in the UV to observe the prototypical X-ray pulsar Her X-1 and its companion HZ Her. Optical spectra were also obtained contemporaneously at the Kitt... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_22955309" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The Faint Object Spectrograph (FOS) aboard Hubble Space Telescope (HST) has been used in the UV to observe the prototypical X-ray pulsar Her X-1 and its companion HZ Her. Optical spectra were also obtained contemporaneously at the Kitt Peak National Observatory (KPNO) 2.1 m. The FOS spectra encompass the 1150-3300 A range near binary orbital phases 0.5 (X-ray maximum) and</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/22955309" 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="b5f4c0cdf419153fa4963e405888ccda" rel="nofollow" data-download="{"attachment_id":43476567,"asset_id":22955309,"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/43476567/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="44652820" href="https://independent.academia.edu/BruceMargon">Bruce Margon</a><script data-card-contents-for-user="44652820" type="text/json">{"id":44652820,"first_name":"Bruce","last_name":"Margon","domain_name":"independent","page_name":"BruceMargon","display_name":"Bruce Margon","profile_url":"https://independent.academia.edu/BruceMargon?f_ri=723","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_22955309 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="22955309"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 22955309, container: ".js-paper-rank-work_22955309", }); 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Optical spectra were also obtained contemporaneously at the Kitt Peak National Observatory (KPNO) 2.1 m. The FOS spectra encompass the 1150-3300 A range near binary orbital phases 0.5 (X-ray maximum) and","downloadable_attachments":[{"id":43476567,"asset_id":22955309,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":44652820,"first_name":"Bruce","last_name":"Margon","domain_name":"independent","page_name":"BruceMargon","display_name":"Bruce Margon","profile_url":"https://independent.academia.edu/BruceMargon?f_ri=723","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":5427,"name":"Spectroscopy","url":"https://www.academia.edu/Documents/in/Spectroscopy?f_ri=723","nofollow":false},{"id":56001,"name":"X 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type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="4362" href="https://www.academia.edu/Documents/in/Protoplanetary_Disks">Protoplanetary Disks</a>, <script data-card-contents-for-ri="4362" type="text/json">{"id":4362,"name":"Protoplanetary Disks","url":"https://www.academia.edu/Documents/in/Protoplanetary_Disks?f_ri=723","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=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=47212539]'), work: {"id":47212539,"title":"The 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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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="721" href="https://www.academia.edu/Documents/in/Magnetohydrodynamics">Magnetohydrodynamics</a>, <script data-card-contents-for-ri="721" type="text/json">{"id":721,"name":"Magnetohydrodynamics","url":"https://www.academia.edu/Documents/in/Magnetohydrodynamics?f_ri=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="45973" href="https://www.academia.edu/Documents/in/Accretion_Disks">Accretion Disks</a><script data-card-contents-for-ri="45973" type="text/json">{"id":45973,"name":"Accretion Disks","url":"https://www.academia.edu/Documents/in/Accretion_Disks?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4380130]'), work: {"id":4380130,"title":"Local Radiative Hydrodynamic and Magnetohydrodynamic Instabilities in Optically Thick 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As anticipated in a recent letter, our results show that although a dual-jet structure is present, the associated luminosity is 100 times smaller than the total one, which is predominantly quadrupolar. We here discuss the details of our implementation of the equations in which the force-free condition is not implemented at a discrete level, but rather obtained via a damping scheme which drives the solution to satisfy the correct condition. We show that this is important for a correct and accurate description of the current sheets that can develop in the course of the simulation. We also study in greater detail the three-dimensional charge distribution produced as a consequence of the inspiral and show that during the inspiral it possesses a complex...</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/71617439" 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="67ec8676d25ebf5afd73e1223ca98ba3" rel="nofollow" data-download="{"attachment_id":80884402,"asset_id":71617439,"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/80884402/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="112942113" href="https://independent.academia.edu/DanielaAlic">Daniela Alic</a><script data-card-contents-for-user="112942113" type="text/json">{"id":112942113,"first_name":"Daniela","last_name":"Alic","domain_name":"independent","page_name":"DanielaAlic","display_name":"Daniela Alic","profile_url":"https://independent.academia.edu/DanielaAlic?f_ri=723","photo":"https://0.academia-photos.com/112942113/26914010/25371205/s65_daniela.alic.jpg"}</script></span></span></li><li class="js-paper-rank-work_71617439 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="71617439"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 71617439, container: ".js-paper-rank-work_71617439", }); 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$(".js-view-count[data-work-id=71617439]").text(description); $(".js-view-count-work_71617439").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_71617439").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="71617439"><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="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=723","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=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=71617439]'), work: {"id":71617439,"title":"Accurate Simulations of Binary Black-Hole Mergers in Force-Free Electrodynamics","created_at":"2022-02-15T07:47:39.463-08:00","url":"https://www.academia.edu/71617439/Accurate_Simulations_of_Binary_Black_Hole_Mergers_in_Force_Free_Electrodynamics?f_ri=723","dom_id":"work_71617439","summary":"We provide additional information on our recent study of the electromagnetic emission produced during the inspiral and merger of supermassive black holes when these are immersed in a force-free plasma threaded by a uniform magnetic field. As anticipated in a recent letter, our results show that although a dual-jet structure is present, the associated luminosity is 100 times smaller than the total one, which is predominantly quadrupolar. We here discuss the details of our implementation of the equations in which the force-free condition is not implemented at a discrete level, but rather obtained via a damping scheme which drives the solution to satisfy the correct condition. We show that this is important for a correct and accurate description of the current sheets that can develop in the course of the simulation. We also study in greater detail the three-dimensional charge distribution produced as a consequence of the inspiral and show that during the inspiral it possesses a complex...","downloadable_attachments":[{"id":80884402,"asset_id":71617439,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":112942113,"first_name":"Daniela","last_name":"Alic","domain_name":"independent","page_name":"DanielaAlic","display_name":"Daniela Alic","profile_url":"https://independent.academia.edu/DanielaAlic?f_ri=723","photo":"https://0.academia-photos.com/112942113/26914010/25371205/s65_daniela.alic.jpg"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","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_70395334" data-work_id="70395334" 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/70395334/Gas_phase_Synthesis_of_Precursors_of_Interstellar_Glycine_A_Computational_Study_of_the_Reactions_of_Acetic_Acid_with_Hydroxylamine_and_Its_Ionized_and_Protonated_">Gas-phase Synthesis of Precursors of Interstellar Glycine: A Computational Study of the Reactions of Acetic Acid with Hydroxylamine and Its Ionized and Protonated …</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/70395334" 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="0c6ebc9f10486865f7235339dd333e99" rel="nofollow" data-download="{"attachment_id":80166608,"asset_id":70395334,"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/80166608/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="33187885" href="https://independent.academia.edu/CBarrientos1">C. 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Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="30329" href="https://www.academia.edu/Documents/in/Genetic_Algorithm">Genetic Algorithm</a>, <script data-card-contents-for-ri="30329" type="text/json">{"id":30329,"name":"Genetic Algorithm","url":"https://www.academia.edu/Documents/in/Genetic_Algorithm?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="158186" href="https://www.academia.edu/Documents/in/Time_Resolved">Time Resolved</a><script data-card-contents-for-ri="158186" type="text/json">{"id":158186,"name":"Time Resolved","url":"https://www.academia.edu/Documents/in/Time_Resolved?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=9564997]'), work: {"id":9564997,"title":"Detection of p-Mode Pulsations and Possible Ellipsoidal 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href="https://www.academia.edu/32454255/A_Single_Circumstellar_Disk_in_the_SVS_13_Close_Binary_System">A Single Circumstellar Disk in the SVS 13 Close Binary System</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/32454255" 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="d67ceab308ba55f1b42f2b141f94ef7d" rel="nofollow" data-download="{"attachment_id":52644326,"asset_id":32454255,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen 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class="InlineList-item-text" data-has-card-for-ri="195544" href="https://www.academia.edu/Documents/in/Planetary_Systems">Planetary Systems</a>, <script data-card-contents-for-ri="195544" type="text/json">{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="1709249" href="https://www.academia.edu/Documents/in/Very_Large_Array">Very Large Array</a><script data-card-contents-for-ri="1709249" type="text/json">{"id":1709249,"name":"Very Large Array","url":"https://www.academia.edu/Documents/in/Very_Large_Array?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=32454255]'), work: {"id":32454255,"title":"A Single Circumstellar Disk in the SVS 13 Close Binary 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Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=723","nofollow":false},{"id":1709249,"name":"Very Large Array","url":"https://www.academia.edu/Documents/in/Very_Large_Array?f_ri=723","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_7988766" data-work_id="7988766" 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/7988766/The_Time_Delay_of_the_Quadruple_Quasar_RX_J0911_4_0551">The Time Delay of the Quadruple Quasar RX J0911.4+0551</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 optical lightcurves of the gravitationally lensed components A (=A1+A2+A3) and B of the quadruple quasar RX J0911.4+0551 (z = 2.80). The observations were primarily obtained at the Nordic Optical Telescope between 1997 March... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_7988766" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present optical lightcurves of the gravitationally lensed components A (=A1+A2+A3) and B of the quadruple quasar RX J0911.4+0551 (z = 2.80). The observations were primarily obtained at the Nordic Optical Telescope between 1997 March and 2001 April and consist of 74 I-band data points for each component. The data allow the measurement of a time delay of 146 +- 8 days (2 sigma) between A and B, with B as the leading component. This value is significantly shorter than that predicted from simple models and indicates a very large external shear. Mass models including the main lens galaxy and the surrounding massive cluster of galaxies at z = 0.77, responsible for the external shear, yield H_0 = 71 +- 4 (random, 2 sigma) +- 8 (systematic) km/s/Mpc. The systematic model uncertainty is governed by the surface-mass density (convergence) at the location of the multiple images.</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/7988766" 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="f4d500a2b39e5aea90f3a2046262b33a" rel="nofollow" data-download="{"attachment_id":34455922,"asset_id":7988766,"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/34455922/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="15267390" href="https://umb.academia.edu/IngunnBurud">Ingunn Burud</a><script data-card-contents-for-user="15267390" type="text/json">{"id":15267390,"first_name":"Ingunn","last_name":"Burud","domain_name":"umb","page_name":"IngunnBurud","display_name":"Ingunn Burud","profile_url":"https://umb.academia.edu/IngunnBurud?f_ri=723","photo":"https://0.academia-photos.com/15267390/139646304/129125358/s65_ingunn.burud.jpeg"}</script></span></span></li><li class="js-paper-rank-work_7988766 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="7988766"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 7988766, container: ".js-paper-rank-work_7988766", }); 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$(".js-view-count[data-work-id=7988766]").text(description); $(".js-view-count-work_7988766").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_7988766").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="7988766"><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="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=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="4564" href="https://www.academia.edu/Documents/in/Observational_Cosmology">Observational Cosmology</a>, <script data-card-contents-for-ri="4564" type="text/json">{"id":4564,"name":"Observational Cosmology","url":"https://www.academia.edu/Documents/in/Observational_Cosmology?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="339537" href="https://www.academia.edu/Documents/in/Model_Uncertainty">Model Uncertainty</a><script data-card-contents-for-ri="339537" type="text/json">{"id":339537,"name":"Model Uncertainty","url":"https://www.academia.edu/Documents/in/Model_Uncertainty?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=7988766]'), work: {"id":7988766,"title":"The Time Delay of the Quadruple Quasar RX J0911.4+0551","created_at":"2014-08-16T00:05:29.912-07:00","url":"https://www.academia.edu/7988766/The_Time_Delay_of_the_Quadruple_Quasar_RX_J0911_4_0551?f_ri=723","dom_id":"work_7988766","summary":"We present optical lightcurves of the gravitationally lensed components A (=A1+A2+A3) and B of the quadruple quasar RX J0911.4+0551 (z = 2.80). The observations were primarily obtained at the Nordic Optical Telescope between 1997 March and 2001 April and consist of 74 I-band data points for each component. The data allow the measurement of a time delay of 146 +- 8 days (2 sigma) between A and B, with B as the leading component. This value is significantly shorter than that predicted from simple models and indicates a very large external shear. Mass models including the main lens galaxy and the surrounding massive cluster of galaxies at z = 0.77, responsible for the external shear, yield H_0 = 71 +- 4 (random, 2 sigma) +- 8 (systematic) km/s/Mpc. The systematic model uncertainty is governed by the surface-mass density (convergence) at the location of the multiple images.","downloadable_attachments":[{"id":34455922,"asset_id":7988766,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":15267390,"first_name":"Ingunn","last_name":"Burud","domain_name":"umb","page_name":"IngunnBurud","display_name":"Ingunn Burud","profile_url":"https://umb.academia.edu/IngunnBurud?f_ri=723","photo":"https://0.academia-photos.com/15267390/139646304/129125358/s65_ingunn.burud.jpeg"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":4564,"name":"Observational Cosmology","url":"https://www.academia.edu/Documents/in/Observational_Cosmology?f_ri=723","nofollow":false},{"id":339537,"name":"Model 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Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":1327,"name":"Convection","url":"https://www.academia.edu/Documents/in/Convection?f_ri=723","nofollow":false},{"id":4107,"name":"High Pressure","url":"https://www.academia.edu/Documents/in/High_Pressure?f_ri=723","nofollow":false},{"id":8067,"name":"Heat Transfer","url":"https://www.academia.edu/Documents/in/Heat_Transfer?f_ri=723"},{"id":40477,"name":"Titan","url":"https://www.academia.edu/Documents/in/Titan?f_ri=723"},{"id":59221,"name":"Phase Diagrams","url":"https://www.academia.edu/Documents/in/Phase_Diagrams?f_ri=723"},{"id":62320,"name":"Dynamics","url":"https://www.academia.edu/Documents/in/Dynamics?f_ri=723"},{"id":66080,"name":"Age","url":"https://www.academia.edu/Documents/in/Age?f_ri=723"},{"id":112334,"name":"Methanol","url":"https://www.academia.edu/Documents/in/Methanol?f_ri=723"},{"id":309434,"name":"Solar System","url":"https://www.academia.edu/Documents/in/Solar_System?f_ri=723"},{"id":604830,"name":"Solar Nebula","url":"https://www.academia.edu/Documents/in/Solar_Nebula?f_ri=723"},{"id":634545,"name":"Condensation","url":"https://www.academia.edu/Documents/in/Condensation?f_ri=723"},{"id":778976,"name":"Scaling Law","url":"https://www.academia.edu/Documents/in/Scaling_Law?f_ri=723"},{"id":881221,"name":"Thermal Convection","url":"https://www.academia.edu/Documents/in/Thermal_Convection?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_2915993" data-work_id="2915993" 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/2915993/The_Prograde_Orbit_of_Exoplanet_TrES_2b">The Prograde Orbit of Exoplanet TrES-2b</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 monitored the Doppler shift of the G0 V star TrES-2 throughout a transit of its giant planet. The anomalous Doppler shift due to stellar rotation (the Rossiter-McLaughlin effect) is discernible in the data, with a signal-to-noise ratio... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_2915993" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We monitored the Doppler shift of the G0 V star TrES-2 throughout a transit of its giant planet. The anomalous Doppler shift due to stellar rotation (the Rossiter-McLaughlin effect) is discernible in the data, with a signal-to-noise ratio of 2.9, even though the star is a slow rotator. By modeling this effect we find that the planet's trajectory across the face of the star is tilted by -9° +/- 12° relative to the projected stellar equator. With 98% confidence, the orbit is prograde. <br />Data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W. M. Keck Foundation.</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/2915993" 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="f85c40d15464fe5c1af8bc3a681267f1" rel="nofollow" data-download="{"attachment_id":34052618,"asset_id":2915993,"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/34052618/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="3429530" href="https://independent.academia.edu/FrancisODonovan">Francis O'Donovan</a><script data-card-contents-for-user="3429530" type="text/json">{"id":3429530,"first_name":"Francis","last_name":"O'Donovan","domain_name":"independent","page_name":"FrancisODonovan","display_name":"Francis O'Donovan","profile_url":"https://independent.academia.edu/FrancisODonovan?f_ri=723","photo":"https://gravatar.com/avatar/21e3405df5e51289ffb5b18f7787d43f?s=65"}</script></span></span></li><li class="js-paper-rank-work_2915993 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="2915993"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 2915993, container: ".js-paper-rank-work_2915993", }); });</script></li><li class="js-percentile-work_2915993 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 = 2915993; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_2915993"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_2915993 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="2915993"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 2915993; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=2915993]").text(description); $(".js-view-count-work_2915993").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_2915993").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="2915993"><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=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="195544" href="https://www.academia.edu/Documents/in/Planetary_Systems">Planetary Systems</a>, <script data-card-contents-for-ri="195544" type="text/json">{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="644390" href="https://www.academia.edu/Documents/in/National_Aeronautics_and_Space_Administration">National Aeronautics and Space Administration</a><script data-card-contents-for-ri="644390" type="text/json">{"id":644390,"name":"National Aeronautics and Space Administration","url":"https://www.academia.edu/Documents/in/National_Aeronautics_and_Space_Administration?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=2915993]'), work: {"id":2915993,"title":"The Prograde Orbit of Exoplanet TrES-2b","created_at":"2013-03-06T01:45:20.979-08:00","url":"https://www.academia.edu/2915993/The_Prograde_Orbit_of_Exoplanet_TrES_2b?f_ri=723","dom_id":"work_2915993","summary":"We monitored the Doppler shift of the G0 V star TrES-2 throughout a transit of its giant planet. The anomalous Doppler shift due to stellar rotation (the Rossiter-McLaughlin effect) is discernible in the data, with a signal-to-noise ratio of 2.9, even though the star is a slow rotator. By modeling this effect we find that the planet's trajectory across the face of the star is tilted by -9° +/- 12° relative to the projected stellar equator. With 98% confidence, the orbit is prograde.\r\nData presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W. M. Keck Foundation.","downloadable_attachments":[{"id":34052618,"asset_id":2915993,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":3429530,"first_name":"Francis","last_name":"O'Donovan","domain_name":"independent","page_name":"FrancisODonovan","display_name":"Francis O'Donovan","profile_url":"https://independent.academia.edu/FrancisODonovan?f_ri=723","photo":"https://gravatar.com/avatar/21e3405df5e51289ffb5b18f7787d43f?s=65"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=723","nofollow":false},{"id":644390,"name":"National Aeronautics and Space Administration","url":"https://www.academia.edu/Documents/in/National_Aeronautics_and_Space_Administration?f_ri=723","nofollow":false},{"id":734113,"name":"University of Southern California","url":"https://www.academia.edu/Documents/in/University_of_Southern_California?f_ri=723"},{"id":991311,"name":"Signal to Noise Ratio","url":"https://www.academia.edu/Documents/in/Signal_to_Noise_Ratio?f_ri=723"},{"id":2331976,"name":"Doppler shift","url":"https://www.academia.edu/Documents/in/Doppler_shift?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_39499345" data-work_id="39499345" 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/39499345/Debye_length_cannot_be_interpreted_as_screening_or_shielding_length">Debye length cannot be interpreted as screening or shielding length</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">This study raises doubts about some fundamental ideas of electrostatics, namely the uniqueness theorems. The Poisson-Boltzmann equation (PBE) gives us very simple formula for charge density distribution (ρe) within fluids. Here we show... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_39499345" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">This study raises doubts about some fundamental ideas of electrostatics, namely the uniqueness theorems. The Poisson-Boltzmann equation (PBE) gives us very simple formula for charge density distribution (ρe) within fluids. Here we show that the old boundary conditions (BC), which are usually used to solve PBE, have serious defects. For example, Dirichlet condition (DC) assigns values to electrostatic potential (ψ) at different boundaries in an absolute sense i.e. without specifying any reference, which is meaningless and leads to violation of charge conservation principle. The Neumann condition (NC) assigns 'independent' values to ψ at different boundaries, whereas they are actually 'related' to each other through Poisson's equation in electrostatics (PES), which makes the solutions non-unique. We use BCs of mixed type to derive correct formula for ρe that addresses the above defects. A remarkable conclusion follows: the present physical interpretation of 'Debye length' (λD) as a screening length is incorrect.</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/39499345" 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="4dd4dbd0534ecadc4e1d9484db8fcc23" rel="nofollow" data-download="{"attachment_id":59647110,"asset_id":39499345,"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/59647110/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="8823428" href="https://iitkgp.academia.edu/RajibChakraborty">Rajib Chakraborty</a><script data-card-contents-for-user="8823428" type="text/json">{"id":8823428,"first_name":"Rajib","last_name":"Chakraborty","domain_name":"iitkgp","page_name":"RajibChakraborty","display_name":"Rajib Chakraborty","profile_url":"https://iitkgp.academia.edu/RajibChakraborty?f_ri=723","photo":"https://0.academia-photos.com/8823428/3208438/8192304/s65_rajib.chakraborty.jpg"}</script></span></span></li><li class="js-paper-rank-work_39499345 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="39499345"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 39499345, container: ".js-paper-rank-work_39499345", }); });</script></li><li class="js-percentile-work_39499345 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 = 39499345; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_39499345"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_39499345 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="39499345"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 39499345; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=39499345]").text(description); $(".js-view-count-work_39499345").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_39499345").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="39499345"><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="517" href="https://www.academia.edu/Documents/in/Plasma_Physics">Plasma Physics</a>, <script data-card-contents-for-ri="517" type="text/json">{"id":517,"name":"Plasma Physics","url":"https://www.academia.edu/Documents/in/Plasma_Physics?f_ri=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="2328" href="https://www.academia.edu/Documents/in/Soft_Condensed_Matter_Physics">Soft Condensed Matter Physics</a>, <script data-card-contents-for-ri="2328" type="text/json">{"id":2328,"name":"Soft Condensed Matter Physics","url":"https://www.academia.edu/Documents/in/Soft_Condensed_Matter_Physics?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="3746" href="https://www.academia.edu/Documents/in/Colloids_and_Surfaces">Colloids and Surfaces</a><script data-card-contents-for-ri="3746" type="text/json">{"id":3746,"name":"Colloids and Surfaces","url":"https://www.academia.edu/Documents/in/Colloids_and_Surfaces?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=39499345]'), work: {"id":39499345,"title":"Debye length cannot be interpreted as screening or shielding length","created_at":"2019-06-10T03:37:43.424-07:00","url":"https://www.academia.edu/39499345/Debye_length_cannot_be_interpreted_as_screening_or_shielding_length?f_ri=723","dom_id":"work_39499345","summary":"This study raises doubts about some fundamental ideas of electrostatics, namely the uniqueness theorems. The Poisson-Boltzmann equation (PBE) gives us very simple formula for charge density distribution (ρe) within fluids. Here we show that the old boundary conditions (BC), which are usually used to solve PBE, have serious defects. For example, Dirichlet condition (DC) assigns values to electrostatic potential (ψ) at different boundaries in an absolute sense i.e. without specifying any reference, which is meaningless and leads to violation of charge conservation principle. The Neumann condition (NC) assigns 'independent' values to ψ at different boundaries, whereas they are actually 'related' to each other through Poisson's equation in electrostatics (PES), which makes the solutions non-unique. We use BCs of mixed type to derive correct formula for ρe that addresses the above defects. A remarkable conclusion follows: the present physical interpretation of 'Debye length' (λD) as a screening length is incorrect.","downloadable_attachments":[{"id":59647110,"asset_id":39499345,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":8823428,"first_name":"Rajib","last_name":"Chakraborty","domain_name":"iitkgp","page_name":"RajibChakraborty","display_name":"Rajib Chakraborty","profile_url":"https://iitkgp.academia.edu/RajibChakraborty?f_ri=723","photo":"https://0.academia-photos.com/8823428/3208438/8192304/s65_rajib.chakraborty.jpg"}],"research_interests":[{"id":517,"name":"Plasma Physics","url":"https://www.academia.edu/Documents/in/Plasma_Physics?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":2328,"name":"Soft Condensed Matter Physics","url":"https://www.academia.edu/Documents/in/Soft_Condensed_Matter_Physics?f_ri=723","nofollow":false},{"id":3746,"name":"Colloids and Surfaces","url":"https://www.academia.edu/Documents/in/Colloids_and_Surfaces?f_ri=723","nofollow":false},{"id":7855,"name":"Plasma Engineering","url":"https://www.academia.edu/Documents/in/Plasma_Engineering?f_ri=723"},{"id":8381,"name":"Electrostatics","url":"https://www.academia.edu/Documents/in/Electrostatics?f_ri=723"},{"id":11671,"name":"Electrokinetics in Nanofluidics","url":"https://www.academia.edu/Documents/in/Electrokinetics_in_Nanofluidics?f_ri=723"},{"id":11672,"name":"Electrokinetics in Microfluidics","url":"https://www.academia.edu/Documents/in/Electrokinetics_in_Microfluidics?f_ri=723"},{"id":16577,"name":"Biological Physics","url":"https://www.academia.edu/Documents/in/Biological_Physics?f_ri=723"},{"id":34910,"name":"Colloidal and Interfacial Phenomena","url":"https://www.academia.edu/Documents/in/Colloidal_and_Interfacial_Phenomena?f_ri=723"},{"id":39579,"name":"Colloid and Interface Chemistry","url":"https://www.academia.edu/Documents/in/Colloid_and_Interface_Chemistry?f_ri=723"},{"id":88562,"name":"Classical Electrodynamics","url":"https://www.academia.edu/Documents/in/Classical_Electrodynamics?f_ri=723"},{"id":135186,"name":"Colloids","url":"https://www.academia.edu/Documents/in/Colloids?f_ri=723"},{"id":317912,"name":"Microfluidics and Nanofluidics","url":"https://www.academia.edu/Documents/in/Microfluidics_and_Nanofluidics?f_ri=723"},{"id":876754,"name":"Tokamak Plasmas","url":"https://www.academia.edu/Documents/in/Tokamak_Plasmas?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_71718457" data-work_id="71718457" 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/71718457/Standard_and_Non_Standard_Plasma_Neutrino_Emission_Revisited">Standard and Non-Standard Plasma Neutrino Emission Revisited</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">On the basis of Braaten and Segel&#x27;s representation of the electro-magnetic dispersion relations in a QED plasma we check the numerical accuracy of several published analytic approximations to the plasma neutrino emission rates. As we... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_71718457" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">On the basis of Braaten and Segel&#x27;s representation of the electro-magnetic dispersion relations in a QED plasma we check the numerical accuracy of several published analytic approximations to the plasma neutrino emission rates. As we find none of them satisfactory we de-rive a ...</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/71718457" 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="9df8c0509c8b0eee74dca5a5ad17fb08" rel="nofollow" data-download="{"attachment_id":80945762,"asset_id":71718457,"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/80945762/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="40984418" href="https://independent.academia.edu/GeorgRaffelt">Georg Raffelt</a><script data-card-contents-for-user="40984418" type="text/json">{"id":40984418,"first_name":"Georg","last_name":"Raffelt","domain_name":"independent","page_name":"GeorgRaffelt","display_name":"Georg Raffelt","profile_url":"https://independent.academia.edu/GeorgRaffelt?f_ri=723","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_71718457 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="71718457"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 71718457, container: ".js-paper-rank-work_71718457", }); });</script></li><li class="js-percentile-work_71718457 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 = 71718457; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_71718457"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_71718457 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="71718457"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 71718457; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=71718457]").text(description); $(".js-view-count-work_71718457").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_71718457").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="71718457"><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="517" href="https://www.academia.edu/Documents/in/Plasma_Physics">Plasma Physics</a>, <script data-card-contents-for-ri="517" type="text/json">{"id":517,"name":"Plasma Physics","url":"https://www.academia.edu/Documents/in/Plasma_Physics?f_ri=723","nofollow":false}</script><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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="712" href="https://www.academia.edu/Documents/in/Stellar_Evolution">Stellar Evolution</a>, <script data-card-contents-for-ri="712" type="text/json">{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=723","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=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=71718457]'), work: {"id":71718457,"title":"Standard and Non-Standard Plasma Neutrino Emission Revisited","created_at":"2022-02-16T18:46:47.394-08:00","url":"https://www.academia.edu/71718457/Standard_and_Non_Standard_Plasma_Neutrino_Emission_Revisited?f_ri=723","dom_id":"work_71718457","summary":"On the basis of Braaten and Segel\u0026#x27;s representation of the electro-magnetic dispersion relations in a QED plasma we check the numerical accuracy of several published analytic approximations to the plasma neutrino emission rates. As we find none of them satisfactory we de-rive a ...","downloadable_attachments":[{"id":80945762,"asset_id":71718457,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":40984418,"first_name":"Georg","last_name":"Raffelt","domain_name":"independent","page_name":"GeorgRaffelt","display_name":"Georg Raffelt","profile_url":"https://independent.academia.edu/GeorgRaffelt?f_ri=723","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":517,"name":"Plasma Physics","url":"https://www.academia.edu/Documents/in/Plasma_Physics?f_ri=723","nofollow":false},{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":2713,"name":"Quantum Electrodynamics","url":"https://www.academia.edu/Documents/in/Quantum_Electrodynamics?f_ri=723"},{"id":12022,"name":"Numerical Analysis","url":"https://www.academia.edu/Documents/in/Numerical_Analysis?f_ri=723"},{"id":45708,"name":"Plasma Processing","url":"https://www.academia.edu/Documents/in/Plasma_Processing?f_ri=723"},{"id":45711,"name":"Computational Astrophysics","url":"https://www.academia.edu/Documents/in/Computational_Astrophysics?f_ri=723"},{"id":151145,"name":"Dispersion Relation","url":"https://www.academia.edu/Documents/in/Dispersion_Relation?f_ri=723"},{"id":181850,"name":"Approximation","url":"https://www.academia.edu/Documents/in/Approximation?f_ri=723"},{"id":386308,"name":"Emission Spectra","url":"https://www.academia.edu/Documents/in/Emission_Spectra?f_ri=723"},{"id":1765696,"name":"Neutrinos","url":"https://www.academia.edu/Documents/in/Neutrinos?f_ri=723"},{"id":2467646,"name":"Emission rate","url":"https://www.academia.edu/Documents/in/Emission_rate?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_33661012" data-work_id="33661012" 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/33661012/Stellar_Metallicities_and_Kinematics_in_a_Gas_Rich_Dwarf_Galaxy_First_Calcium_Triplet_Spectroscopy_of_Red_Giant_Branch_Stars_in_WLM">Stellar Metallicities and Kinematics in a Gas-Rich Dwarf Galaxy: First Calcium Triplet Spectroscopy of Red Giant Branch Stars in WLM</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/33661012" data-share-source="work_strip" 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itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="65895241" href="https://independent.academia.edu/EvanSkillman">Evan Skillman</a><script data-card-contents-for-user="65895241" type="text/json">{"id":65895241,"first_name":"Evan","last_name":"Skillman","domain_name":"independent","page_name":"EvanSkillman","display_name":"Evan Skillman","profile_url":"https://independent.academia.edu/EvanSkillman?f_ri=723","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_33661012 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="33661012"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 33661012, container: ".js-paper-rank-work_33661012", }); });</script></li><li class="js-percentile-work_33661012 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 = 33661012; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_33661012"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_33661012 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="33661012"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 33661012; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=33661012]").text(description); $(".js-view-count-work_33661012").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_33661012").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="33661012"><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="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=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="5427" href="https://www.academia.edu/Documents/in/Spectroscopy">Spectroscopy</a>, <script data-card-contents-for-ri="5427" type="text/json">{"id":5427,"name":"Spectroscopy","url":"https://www.academia.edu/Documents/in/Spectroscopy?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="11050" href="https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution">Galaxy Formation and Evolution</a><script data-card-contents-for-ri="11050" type="text/json">{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=33661012]'), work: {"id":33661012,"title":"Stellar Metallicities and Kinematics in a Gas-Rich Dwarf Galaxy: First Calcium Triplet Spectroscopy of Red Giant Branch Stars in WLM","created_at":"2017-06-26T09:48:55.731-07:00","url":"https://www.academia.edu/33661012/Stellar_Metallicities_and_Kinematics_in_a_Gas_Rich_Dwarf_Galaxy_First_Calcium_Triplet_Spectroscopy_of_Red_Giant_Branch_Stars_in_WLM?f_ri=723","dom_id":"work_33661012","summary":null,"downloadable_attachments":[{"id":53668666,"asset_id":33661012,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":65895241,"first_name":"Evan","last_name":"Skillman","domain_name":"independent","page_name":"EvanSkillman","display_name":"Evan Skillman","profile_url":"https://independent.academia.edu/EvanSkillman?f_ri=723","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":5427,"name":"Spectroscopy","url":"https://www.academia.edu/Documents/in/Spectroscopy?f_ri=723","nofollow":false},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=723","nofollow":false},{"id":62320,"name":"Dynamics","url":"https://www.academia.edu/Documents/in/Dynamics?f_ri=723"},{"id":69841,"name":"Standard Deviation","url":"https://www.academia.edu/Documents/in/Standard_Deviation?f_ri=723"},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=723"},{"id":106861,"name":"Dwarf Galaxies","url":"https://www.academia.edu/Documents/in/Dwarf_Galaxies?f_ri=723"},{"id":119118,"name":"Age Estimation","url":"https://www.academia.edu/Documents/in/Age_Estimation?f_ri=723"},{"id":151974,"name":"Abundance","url":"https://www.academia.edu/Documents/in/Abundance?f_ri=723"},{"id":174322,"name":"Kinematics and Dynamics","url":"https://www.academia.edu/Documents/in/Kinematics_and_Dynamics?f_ri=723"},{"id":194426,"name":"Radial Velocity","url":"https://www.academia.edu/Documents/in/Radial_Velocity?f_ri=723"},{"id":966637,"name":"Rotation Curve","url":"https://www.academia.edu/Documents/in/Rotation_Curve?f_ri=723"},{"id":1140559,"name":"Field of View","url":"https://www.academia.edu/Documents/in/Field_of_View?f_ri=723"},{"id":1403430,"name":"Stellar Kinematics","url":"https://www.academia.edu/Documents/in/Stellar_Kinematics?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_74572028" data-work_id="74572028" 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/74572028/A_Giant_Outburst_at_Millimeter_Wavelengths_in_the_Orion_Nebula">A Giant Outburst at Millimeter Wavelengths in the Orion Nebula</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">BIMA observations of the Orion nebula discovered a giant flare from a young star previously undetected at millimeter wavelengths. The star briefly became the brightest compact object in the nebula at 86 GHz. Its flux density increased by... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_74572028" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">BIMA observations of the Orion nebula discovered a giant flare from a young star previously undetected at millimeter wavelengths. The star briefly became the brightest compact object in the nebula at 86 GHz. Its flux density increased by more than a factor of 5 on a timescale of hours, to a peak of 160 mJy. This is one of the most luminous stellar radio flares ever observed. Remarkably, the Chandra X-ray observatory was in the midst of a deep integration of the Orion nebula at the time of the BIMA discovery; the source&#39;s X-ray flux increased by a factor of 10 approximately 2 days before the radio detection. Follow-up radio observations with the VLA and BIMA showed that the source decayed on a timescale of days, then flared again several times over the next 70 days, although never as brightly as during the discovery. Circular polarization was detected at 15, 22, and 43 GHz, indicating that the emission mechanism was cyclotron. VLBA observations 9 days after the initial flare yiel...</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/74572028" 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="9852db5d13ba9486700e4ca586391640" rel="nofollow" data-download="{"attachment_id":82676907,"asset_id":74572028,"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/82676907/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="210239555" href="https://mit.academia.edu/FrederickBaganoff">Frederick K Baganoff</a><script data-card-contents-for-user="210239555" type="text/json">{"id":210239555,"first_name":"Frederick","last_name":"Baganoff","domain_name":"mit","page_name":"FrederickBaganoff","display_name":"Frederick K Baganoff","profile_url":"https://mit.academia.edu/FrederickBaganoff?f_ri=723","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_74572028 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="74572028"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 74572028, container: ".js-paper-rank-work_74572028", }); 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$(".js-view-count[data-work-id=74572028]").text(description); $(".js-view-count-work_74572028").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_74572028").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="74572028"><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="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=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="56001" href="https://www.academia.edu/Documents/in/X_Rays">X Rays</a>, <script data-card-contents-for-ri="56001" type="text/json">{"id":56001,"name":"X Rays","url":"https://www.academia.edu/Documents/in/X_Rays?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="78842" href="https://www.academia.edu/Documents/in/Infrared_spectroscopy">Infrared spectroscopy</a><script data-card-contents-for-ri="78842" type="text/json">{"id":78842,"name":"Infrared spectroscopy","url":"https://www.academia.edu/Documents/in/Infrared_spectroscopy?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=74572028]'), work: {"id":74572028,"title":"A Giant Outburst at Millimeter Wavelengths in the Orion Nebula","created_at":"2022-03-25T14:21:36.329-07:00","url":"https://www.academia.edu/74572028/A_Giant_Outburst_at_Millimeter_Wavelengths_in_the_Orion_Nebula?f_ri=723","dom_id":"work_74572028","summary":"BIMA observations of the Orion nebula discovered a giant flare from a young star previously undetected at millimeter wavelengths. The star briefly became the brightest compact object in the nebula at 86 GHz. Its flux density increased by more than a factor of 5 on a timescale of hours, to a peak of 160 mJy. This is one of the most luminous stellar radio flares ever observed. Remarkably, the Chandra X-ray observatory was in the midst of a deep integration of the Orion nebula at the time of the BIMA discovery; the source\u0026#39;s X-ray flux increased by a factor of 10 approximately 2 days before the radio detection. Follow-up radio observations with the VLA and BIMA showed that the source decayed on a timescale of days, then flared again several times over the next 70 days, although never as brightly as during the discovery. Circular polarization was detected at 15, 22, and 43 GHz, indicating that the emission mechanism was cyclotron. VLBA observations 9 days after the initial flare yiel...","downloadable_attachments":[{"id":82676907,"asset_id":74572028,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":210239555,"first_name":"Frederick","last_name":"Baganoff","domain_name":"mit","page_name":"FrederickBaganoff","display_name":"Frederick K Baganoff","profile_url":"https://mit.academia.edu/FrederickBaganoff?f_ri=723","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":56001,"name":"X Rays","url":"https://www.academia.edu/Documents/in/X_Rays?f_ri=723","nofollow":false},{"id":78842,"name":"Infrared spectroscopy","url":"https://www.academia.edu/Documents/in/Infrared_spectroscopy?f_ri=723","nofollow":false},{"id":321836,"name":"Spectrum","url":"https://www.academia.edu/Documents/in/Spectrum?f_ri=723"},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=723"},{"id":2193830,"name":"Brightness temperature","url":"https://www.academia.edu/Documents/in/Brightness_temperature?f_ri=723"},{"id":2477780,"name":"Circular polarization","url":"https://www.academia.edu/Documents/in/Circular_polarization?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_69190569" data-work_id="69190569" 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/69190569/s_Process_Nucleosynthesis_in_Advanced_Burning_Phases_of_Massive_Stars">s-Process Nucleosynthesis in Advanced Burning Phases of Massive 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">We present a detailed study of s-process nucleosynthesis in massive stars of solar-like initial composition and masses 15, 20, 25, and 30 M⊙. We update our previous results of s-process nucleosynthesis during the core He-burning of these... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_69190569" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present a detailed study of s-process nucleosynthesis in massive stars of solar-like initial composition and masses 15, 20, 25, and 30 M⊙. We update our previous results of s-process nucleosynthesis during the core He-burning of these stars and then focus on an analysis of the s-process under the physical conditions encountered during the shell-carbon burning. We show that the recent compilation of the 22 Ne(α, n) 25 Mg rate leads to a remarkable reduction of the efficiency of the s-process during core He-burning. In particular, this rate leads to the lowest overproduction factor of 80 Kr found to date during core He-burning in massive stars. The s-process yields resulting from shell carbon burning turn out to be very sensitive to the structural evolution of the carbon shell. This structure is influenced by the mass fraction of 12 C attained at the end of core helium burning, which in turn is mainly determined by the 12 C(α, γ) 16 O reaction. The still present uncertainty in the ...</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/69190569" 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="f4a018106e9236b6c99e1a869ff71cde" rel="nofollow" data-download="{"attachment_id":79380195,"asset_id":69190569,"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/79380195/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="184651676" href="https://independent.academia.edu/MounibElEid">Mounib El Eid</a><script data-card-contents-for-user="184651676" type="text/json">{"id":184651676,"first_name":"Mounib","last_name":"El Eid","domain_name":"independent","page_name":"MounibElEid","display_name":"Mounib El Eid","profile_url":"https://independent.academia.edu/MounibElEid?f_ri=723","photo":"https://0.academia-photos.com/184651676/118088564/107396556/s65_mounib.el_eid.jpeg"}</script></span></span></li><li class="js-paper-rank-work_69190569 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="69190569"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 69190569, container: ".js-paper-rank-work_69190569", }); 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$(".js-view-count[data-work-id=69190569]").text(description); $(".js-view-count-work_69190569").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_69190569").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="69190569"><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="422" href="https://www.academia.edu/Documents/in/Computer_Science">Computer Science</a>, <script data-card-contents-for-ri="422" type="text/json">{"id":422,"name":"Computer Science","url":"https://www.academia.edu/Documents/in/Computer_Science?f_ri=723","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=723","nofollow":false}</script><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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="712" href="https://www.academia.edu/Documents/in/Stellar_Evolution">Stellar Evolution</a><script data-card-contents-for-ri="712" type="text/json">{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=69190569]'), work: {"id":69190569,"title":"s-Process Nucleosynthesis in Advanced Burning Phases of Massive Stars","created_at":"2022-01-22T11:53:08.427-08:00","url":"https://www.academia.edu/69190569/s_Process_Nucleosynthesis_in_Advanced_Burning_Phases_of_Massive_Stars?f_ri=723","dom_id":"work_69190569","summary":"We present a detailed study of s-process nucleosynthesis in massive stars of solar-like initial composition and masses 15, 20, 25, and 30 M⊙. We update our previous results of s-process nucleosynthesis during the core He-burning of these stars and then focus on an analysis of the s-process under the physical conditions encountered during the shell-carbon burning. We show that the recent compilation of the 22 Ne(α, n) 25 Mg rate leads to a remarkable reduction of the efficiency of the s-process during core He-burning. In particular, this rate leads to the lowest overproduction factor of 80 Kr found to date during core He-burning in massive stars. The s-process yields resulting from shell carbon burning turn out to be very sensitive to the structural evolution of the carbon shell. This structure is influenced by the mass fraction of 12 C attained at the end of core helium burning, which in turn is mainly determined by the 12 C(α, γ) 16 O reaction. The still present uncertainty in the ...","downloadable_attachments":[{"id":79380195,"asset_id":69190569,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":184651676,"first_name":"Mounib","last_name":"El Eid","domain_name":"independent","page_name":"MounibElEid","display_name":"Mounib El Eid","profile_url":"https://independent.academia.edu/MounibElEid?f_ri=723","photo":"https://0.academia-photos.com/184651676/118088564/107396556/s65_mounib.el_eid.jpeg"}],"research_interests":[{"id":422,"name":"Computer Science","url":"https://www.academia.edu/Documents/in/Computer_Science?f_ri=723","nofollow":false},{"id":498,"name":"Physics","url":"https://www.academia.edu/Documents/in/Physics?f_ri=723","nofollow":false},{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723"},{"id":230832,"name":"Nuclear Reactions","url":"https://www.academia.edu/Documents/in/Nuclear_Reactions?f_ri=723"},{"id":2504124,"name":"Nucleosynthesis","url":"https://www.academia.edu/Documents/in/Nucleosynthesis?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_74810173" data-work_id="74810173" 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/74810173/A_Cosmological_Kinetic_Theory_for_the_Evolution_of_Cold_Dark_Matter_Halos_with_Substructure_Quasi_Linear_Theory">A Cosmological Kinetic Theory for the Evolution of Cold Dark Matter Halos with Substructure: Quasi-Linear Theory</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 a kinetic theory for the evolution of the phase-space distribution of dark matter particles in galaxy halos in the presence of a cosmological spectrum of fluctuations. This theory introduces a new way to model the formation and... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_74810173" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present a kinetic theory for the evolution of the phase-space distribution of dark matter particles in galaxy halos in the presence of a cosmological spectrum of fluctuations. This theory introduces a new way to model the formation and evolution of halos, which traditionally have been investigated by analytic gravitational infall models or numerical N-body methods. Unlike the collisionless Boltzmann equation, our kinetic equation contains nonzero terms on the right-hand side arising from stochastic fluctuations in the gravitational potential due to substructures in the dark matter mass distribution. Using statistics for constrained Gaussian random fields in standard cosmological models, we show that our kinetic equation to second-order in perturbation theory is of the Fokker-Planck form, with one scattering term representing drift and the other representing diffusion in velocity-space. The drift is radial, and the drift and diffusion coefficients depend only on positions and not ...</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/74810173" 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="b80bbbe6cf5f5ebec7e86f9a34a19be0" rel="nofollow" data-download="{"attachment_id":82827135,"asset_id":74810173,"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/82827135/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="40879463" href="https://independent.academia.edu/ChungpeiMa">Chung-pei Ma</a><script data-card-contents-for-user="40879463" type="text/json">{"id":40879463,"first_name":"Chung-pei","last_name":"Ma","domain_name":"independent","page_name":"ChungpeiMa","display_name":"Chung-pei Ma","profile_url":"https://independent.academia.edu/ChungpeiMa?f_ri=723","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_74810173 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="74810173"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 74810173, container: ".js-paper-rank-work_74810173", }); 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This theory introduces a new way to model the formation and evolution of halos, which traditionally have been investigated by analytic gravitational infall models or numerical N-body methods. Unlike the collisionless Boltzmann equation, our kinetic equation contains nonzero terms on the right-hand side arising from stochastic fluctuations in the gravitational potential due to substructures in the dark matter mass distribution. Using statistics for constrained Gaussian random fields in standard cosmological models, we show that our kinetic equation to second-order in perturbation theory is of the Fokker-Planck form, with one scattering term representing drift and the other representing diffusion in velocity-space. 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Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":178406,"name":"Gamma Ray Burst","url":"https://www.academia.edu/Documents/in/Gamma_Ray_Burst?f_ri=723","nofollow":false},{"id":875506,"name":"Physical Model","url":"https://www.academia.edu/Documents/in/Physical_Model?f_ri=723","nofollow":false},{"id":3835050,"name":"Exponential Decay","url":"https://www.academia.edu/Documents/in/Exponential_Decay?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_35021358 coauthored" data-work_id="35021358" 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/35021358/Wavelet_Phase_Coherence_Analysis_Application_to_a_Quiet_Sun_Magnetic_Element">Wavelet Phase Coherence 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James McAteer","profile_url":"https://nmsu.academia.edu/RtJamesMcAteer?f_ri=723","photo":"https://gravatar.com/avatar/e85ff9df2198a62ee6da746b2af6d9e1?s=65"},{"id":38841760,"first_name":"Philip","last_name":"Judge","domain_name":"independent","page_name":"PhilipJudge","display_name":"Philip Judge","profile_url":"https://independent.academia.edu/PhilipJudge?f_ri=723","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","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_44445082" data-work_id="44445082" 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/44445082/Introduction_to_Plasma_Physics_and_Controlled_Fusion_by_Francis_F_Chen">Introduction to Plasma Physics and Controlled Fusion by Francis F. Chen</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest">Introduction to Plasma Physics and Controlled Fusion by Francis F. Chen<br /><br />PLENUM PRESS<br />NEW YORK AND LONDON</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/44445082" 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="950ed7a26b8b69e224794b422fa02209" rel="nofollow" data-download="{"attachment_id":64866003,"asset_id":44445082,"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/64866003/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="60888078" href="https://independent.academia.edu/akshay_sb">Akshay SB</a><script data-card-contents-for-user="60888078" type="text/json">{"id":60888078,"first_name":"Akshay","last_name":"SB","domain_name":"independent","page_name":"akshay_sb","display_name":"Akshay SB","profile_url":"https://independent.academia.edu/akshay_sb?f_ri=723","photo":"https://0.academia-photos.com/60888078/15866790/34883599/s65_akshay.sunil_bhadage.jpg"}</script></span></span></li><li class="js-paper-rank-work_44445082 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="44445082"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 44445082, container: ".js-paper-rank-work_44445082", }); 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$(".js-view-count[data-work-id=44445082]").text(description); $(".js-view-count-work_44445082").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_44445082").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="44445082"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">16</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="300" href="https://www.academia.edu/Documents/in/Mathematics">Mathematics</a>, <script data-card-contents-for-ri="300" type="text/json">{"id":300,"name":"Mathematics","url":"https://www.academia.edu/Documents/in/Mathematics?f_ri=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="517" href="https://www.academia.edu/Documents/in/Plasma_Physics">Plasma Physics</a>, <script data-card-contents-for-ri="517" type="text/json">{"id":517,"name":"Plasma Physics","url":"https://www.academia.edu/Documents/in/Plasma_Physics?f_ri=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="518" href="https://www.academia.edu/Documents/in/Quantum_Physics">Quantum Physics</a><script data-card-contents-for-ri="518" type="text/json">{"id":518,"name":"Quantum Physics","url":"https://www.academia.edu/Documents/in/Quantum_Physics?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=44445082]'), work: {"id":44445082,"title":"Introduction to Plasma Physics and Controlled Fusion by Francis F. 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Chen\n\nPLENUM PRESS\nNEW YORK AND LONDON ","downloadable_attachments":[{"id":64866003,"asset_id":44445082,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":60888078,"first_name":"Akshay","last_name":"SB","domain_name":"independent","page_name":"akshay_sb","display_name":"Akshay SB","profile_url":"https://independent.academia.edu/akshay_sb?f_ri=723","photo":"https://0.academia-photos.com/60888078/15866790/34883599/s65_akshay.sunil_bhadage.jpg"}],"research_interests":[{"id":300,"name":"Mathematics","url":"https://www.academia.edu/Documents/in/Mathematics?f_ri=723","nofollow":false},{"id":498,"name":"Physics","url":"https://www.academia.edu/Documents/in/Physics?f_ri=723","nofollow":false},{"id":517,"name":"Plasma Physics","url":"https://www.academia.edu/Documents/in/Plasma_Physics?f_ri=723","nofollow":false},{"id":518,"name":"Quantum Physics","url":"https://www.academia.edu/Documents/in/Quantum_Physics?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723"},{"id":888,"name":"Cosmology (Physics)","url":"https://www.academia.edu/Documents/in/Cosmology_Physics_?f_ri=723"},{"id":2713,"name":"Quantum Electrodynamics","url":"https://www.academia.edu/Documents/in/Quantum_Electrodynamics?f_ri=723"},{"id":2731,"name":"Mathematics Education","url":"https://www.academia.edu/Documents/in/Mathematics_Education?f_ri=723"},{"id":4337,"name":"Space Plasma Physics","url":"https://www.academia.edu/Documents/in/Space_Plasma_Physics?f_ri=723"},{"id":7855,"name":"Plasma Engineering","url":"https://www.academia.edu/Documents/in/Plasma_Engineering?f_ri=723"},{"id":7936,"name":"Quantum Mechanics","url":"https://www.academia.edu/Documents/in/Quantum_Mechanics?f_ri=723"},{"id":17871,"name":"Physics Education","url":"https://www.academia.edu/Documents/in/Physics_Education?f_ri=723"},{"id":42358,"name":"Maxwell's Equations","url":"https://www.academia.edu/Documents/in/Maxwells_Equations?f_ri=723"},{"id":92877,"name":"Electrodynamics","url":"https://www.academia.edu/Documents/in/Electrodynamics?f_ri=723"},{"id":117555,"name":"Plasma","url":"https://www.academia.edu/Documents/in/Plasma?f_ri=723"},{"id":433554,"name":"Jet Propulsion","url":"https://www.academia.edu/Documents/in/Jet_Propulsion?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_7213812" data-work_id="7213812" 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/7213812/Fermi_Large_Area_Telescope_Observations_of_Markarian_421_The_Missing_Piece_of_its_Spectral_Energy_Distribution">Fermi Large Area Telescope Observations of Markarian 421: The Missing Piece of its Spectral Energy Distribution</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 report on the γ-ray activity of the high-synchrotron-peaked BL Lacertae object Markarian 421 (Mrk 421) during the first 1.5 years of Fermi operation, from 2008 August 5 to 2010 March 12. We find that the Large Area Telescope (LAT)... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_7213812" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We report on the γ-ray activity of the high-synchrotron-peaked BL Lacertae object Markarian 421 (Mrk 421) during the first 1.5 years of Fermi operation, from 2008 August 5 to 2010 March 12. We find that the Large Area Telescope (LAT) γ-ray spectrum above 0.3 GeV can be well described by a power-law function with photon index Γ = 1.78 ± 0.02 and average photon flux F(> 0.3 GeV) = (7.23 ± 0.16) × 10-8 ph cm-2 s-1. Over this time period, the Fermi-LAT spectrum above 0.3 GeV was evaluated on seven-day-long time intervals, showing significant variations in the photon flux (up to a factor ~3 from the minimum to the maximum flux) but mild spectral variations. The variability amplitude at X-ray frequencies measured by RXTE/ASM and Swift/BAT is substantially larger than that in γ-rays measured by Fermi-LAT, and these two energy ranges are not significantly correlated. We also present the first results from the 4.5 month long multifrequency campaign on Mrk 421, which included the VLBA, Swift, RXTE, MAGIC, the F-GAMMA, GASP-WEBT, and other collaborations and instruments that provided excellent temporal and energy coverage of the source throughout the entire campaign (2009 January 19 to 2009 June 1). During this campaign, Mrk 421 showed a low activity at all wavebands. The extensive multi-instrument (radio to TeV) data set provides an unprecedented, complete look at the quiescent spectral energy distribution (SED) for this source. The broadband SED was reproduced with a leptonic (one-zone synchrotron self-Compton) and a hadronic model (synchrotron proton blazar). Both frameworks are able to describe the average SED reasonably well, implying comparable jet powers but very different characteristics for the blazar emission site.</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/7213812" 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="976af436281b3e66c59f6dc94ad861b8" rel="nofollow" data-download="{"attachment_id":33837463,"asset_id":7213812,"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/33837463/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="12524756" href="https://independent.academia.edu/ChristianAbrahamCarmonaGonzalez">Christian Abraham Carmona Gonzalez</a><script data-card-contents-for-user="12524756" type="text/json">{"id":12524756,"first_name":"Christian Abraham","last_name":"Carmona Gonzalez","domain_name":"independent","page_name":"ChristianAbrahamCarmonaGonzalez","display_name":"Christian Abraham Carmona Gonzalez","profile_url":"https://independent.academia.edu/ChristianAbrahamCarmonaGonzalez?f_ri=723","photo":"https://0.academia-photos.com/12524756/8918651/9953756/s65_christian_abraham.carmona_gonzalez.jpg_oh_99c363185485f2c5ccab82ba63e81169_oe_55da11e2___gda___1440830585_a4226ae5c7457177c406e4bedafbc4a7"}</script></span></span></li><li class="js-paper-rank-work_7213812 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="7213812"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 7213812, container: ".js-paper-rank-work_7213812", }); 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$(".js-view-count[data-work-id=7213812]").text(description); $(".js-view-count-work_7213812").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_7213812").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="7213812"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">11</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="87" href="https://www.academia.edu/Documents/in/Telecommunications_Engineering">Telecommunications Engineering</a>, <script data-card-contents-for-ri="87" type="text/json">{"id":87,"name":"Telecommunications Engineering","url":"https://www.academia.edu/Documents/in/Telecommunications_Engineering?f_ri=723","nofollow":false}</script><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=723","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=723","nofollow":false}</script><a class="InlineList-item-text" data-has-card-for-ri="56001" href="https://www.academia.edu/Documents/in/X_Rays">X Rays</a><script data-card-contents-for-ri="56001" type="text/json">{"id":56001,"name":"X Rays","url":"https://www.academia.edu/Documents/in/X_Rays?f_ri=723","nofollow":false}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=7213812]'), work: {"id":7213812,"title":"Fermi Large Area Telescope Observations of Markarian 421: The Missing Piece of its Spectral Energy Distribution","created_at":"2014-05-31T04:00:01.133-07:00","url":"https://www.academia.edu/7213812/Fermi_Large_Area_Telescope_Observations_of_Markarian_421_The_Missing_Piece_of_its_Spectral_Energy_Distribution?f_ri=723","dom_id":"work_7213812","summary":"We report on the γ-ray activity of the high-synchrotron-peaked BL Lacertae object Markarian 421 (Mrk 421) during the first 1.5 years of Fermi operation, from 2008 August 5 to 2010 March 12. We find that the Large Area Telescope (LAT) γ-ray spectrum above 0.3 GeV can be well described by a power-law function with photon index Γ = 1.78 ± 0.02 and average photon flux F(\u003e 0.3 GeV) = (7.23 ± 0.16) × 10-8 ph cm-2 s-1. Over this time period, the Fermi-LAT spectrum above 0.3 GeV was evaluated on seven-day-long time intervals, showing significant variations in the photon flux (up to a factor ~3 from the minimum to the maximum flux) but mild spectral variations. The variability amplitude at X-ray frequencies measured by RXTE/ASM and Swift/BAT is substantially larger than that in γ-rays measured by Fermi-LAT, and these two energy ranges are not significantly correlated. We also present the first results from the 4.5 month long multifrequency campaign on Mrk 421, which included the VLBA, Swift, RXTE, MAGIC, the F-GAMMA, GASP-WEBT, and other collaborations and instruments that provided excellent temporal and energy coverage of the source throughout the entire campaign (2009 January 19 to 2009 June 1). During this campaign, Mrk 421 showed a low activity at all wavebands. The extensive multi-instrument (radio to TeV) data set provides an unprecedented, complete look at the quiescent spectral energy distribution (SED) for this source. The broadband SED was reproduced with a leptonic (one-zone synchrotron self-Compton) and a hadronic model (synchrotron proton blazar). Both frameworks are able to describe the average SED reasonably well, implying comparable jet powers but very different characteristics for the blazar emission site.","downloadable_attachments":[{"id":33837463,"asset_id":7213812,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":12524756,"first_name":"Christian Abraham","last_name":"Carmona Gonzalez","domain_name":"independent","page_name":"ChristianAbrahamCarmonaGonzalez","display_name":"Christian Abraham Carmona Gonzalez","profile_url":"https://independent.academia.edu/ChristianAbrahamCarmonaGonzalez?f_ri=723","photo":"https://0.academia-photos.com/12524756/8918651/9953756/s65_christian_abraham.carmona_gonzalez.jpg_oh_99c363185485f2c5ccab82ba63e81169_oe_55da11e2___gda___1440830585_a4226ae5c7457177c406e4bedafbc4a7"}],"research_interests":[{"id":87,"name":"Telecommunications Engineering","url":"https://www.academia.edu/Documents/in/Telecommunications_Engineering?f_ri=723","nofollow":false},{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=723","nofollow":false},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=723","nofollow":false},{"id":56001,"name":"X Rays","url":"https://www.academia.edu/Documents/in/X_Rays?f_ri=723","nofollow":false},{"id":113890,"name":"Power Law","url":"https://www.academia.edu/Documents/in/Power_Law?f_ri=723"},{"id":316011,"name":"BL Lacertae objects","url":"https://www.academia.edu/Documents/in/BL_Lacertae_objects?f_ri=723"},{"id":321836,"name":"Spectrum","url":"https://www.academia.edu/Documents/in/Spectrum?f_ri=723"},{"id":749302,"name":"Indexation","url":"https://www.academia.edu/Documents/in/Indexation?f_ri=723"},{"id":912885,"name":"Gamma Ray","url":"https://www.academia.edu/Documents/in/Gamma_Ray?f_ri=723"},{"id":1607964,"name":"Acceleration of Particles","url":"https://www.academia.edu/Documents/in/Acceleration_of_Particles?f_ri=723"},{"id":2217031,"name":"Spectral Energy Distribution","url":"https://www.academia.edu/Documents/in/Spectral_Energy_Distribution?f_ri=723"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_37490311" data-work_id="37490311" 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/37490311/Plasma_Petroglyphs_Plasmaglyphs_Earthworks_and_the_Megafauna_Extinction">Plasma Petroglyphs (Plasmaglyphs), Earthworks, and the Megafauna Extinction</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 presents an exciting new hypothesis for megafauna extinction based upon historical, mythical, geological, astronomic, and atmospheric evidence. While not conclusive, it is highly compelling and demands further investigation.... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_37490311" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The author presents an exciting new hypothesis for megafauna extinction based upon historical, mythical, geological, astronomic, and atmospheric evidence. While not conclusive, it is highly compelling and demands further investigation. Examples of cross cultural motifs in the form of glyphs, mounds, and earthworks are provided with mythic comparisons and contrasts. Counter arguments are provided throughout as well as strong debunking of prior archaeological biases rooted in Victorian, antiquated pseudoscience. Assumptions in the two models presented for plasma-arc-discharge mechanism are clearly listed, as well as known facts. Citations enable cross reference while the work focuses not on diffusion anthropology, but realistic atmospheric/astronomical plasmoid petroglyph formations recorded in rock</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/37490311" 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="1f7648369604a2ac23af79d4228fef38" rel="nofollow" data-download="{"attachment_id":59041250,"asset_id":37490311,"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/59041250/download_file?st=MTczMjczODUwMyw4LjIyMi4yMDguMTQ2&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="16114743" href="https://uky.academia.edu/ShifuCareaga">Shifu Careaga</a><script data-card-contents-for-user="16114743" type="text/json">{"id":16114743,"first_name":"Shifu","last_name":"Careaga","domain_name":"uky","page_name":"ShifuCareaga","display_name":"Shifu Careaga","profile_url":"https://uky.academia.edu/ShifuCareaga?f_ri=723","photo":"https://0.academia-photos.com/16114743/4461981/27493650/s65_shifu.careaga.jpg"}</script></span></span></li><li class="js-paper-rank-work_37490311 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="37490311"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 37490311, container: ".js-paper-rank-work_37490311", }); 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