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overflow: hidden; text-overflow: ellipsis; -webkit-line-clamp: 3; -webkit-box-orient: vertical; }</style><div class="col-xs-12 clearfix"><div class="u-floatLeft"><h1 class="PageHeader-title u-m0x u-fs30">Star formation (Physics)</h1><div class="u-tcGrayDark">37 Followers</div><div class="u-tcGrayDark u-mt2x">Recent papers in <b>Star formation (Physics)</b></div></div></div></div></div></div><div class="TabbedNavigation"><div class="container"><div class="row"><div class="col-xs-12 clearfix"><ul class="nav u-m0x u-p0x list-inline u-displayFlex"><li class="active"><a href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Top Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Star_formation_Physics_/MostCited">Most Cited Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Star_formation_Physics_/MostDownloaded">Most Downloaded Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Star_formation_Physics_/MostRecent">Newest Papers</a></li><li><a class="" href="https://www.academia.edu/People/Star_formation_Physics_">People</a></li></ul></div><style type="text/css">ul.nav{flex-direction:row}@media(max-width: 567px){ul.nav{flex-direction:column}.TabbedNavigation li{max-width:100%}.TabbedNavigation li.active{background-color:var(--background-grey, #dddde2)}.TabbedNavigation li.active:before,.TabbedNavigation li.active:after{display:none}}</style></div></div></div><div class="container"><div class="row"><div class="col-xs-12"><div class="u-displayFlex"><div class="u-flexGrow1"><div class="works"><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_35538530" data-work_id="35538530" 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/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22">High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_35538530" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 M e Myr −1 , suggesting the hub mass would be doubled in six free-fall times, adding up to ∼2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO + (3–2) and 13 CO(3–2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s −1 and 7.2×10 −4 M e yr −1 , respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11–15 M e and it is still growing with an accretion rate of 7×10 −5 M e yr −1. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.</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/35538530" 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="d30d93dceb6b50d68989eb301426b7d3" rel="nofollow" data-download="{"attachment_id":55404248,"asset_id":35538530,"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/55404248/download_file?st=MTc0MDAzNDU3NCw4LjIyMi4yMDguMTQ2&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="66695878" href="https://gucas.academia.edu/jhyuannaoc">Jinghua Yuan</a><script data-card-contents-for-user="66695878" type="text/json">{"id":66695878,"first_name":"Jinghua","last_name":"Yuan","domain_name":"gucas","page_name":"jhyuannaoc","display_name":"Jinghua Yuan","profile_url":"https://gucas.academia.edu/jhyuannaoc?f_ri=24009","photo":"https://0.academia-photos.com/66695878/17364443/17484885/s65_jinghua.yuan.jpg"}</script></span></span></li><li class="js-paper-rank-work_35538530 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="35538530"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 35538530, container: ".js-paper-rank-work_35538530", }); 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$(".js-view-count[data-work-id=35538530]").text(description); $(".js-view-count-work_35538530").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_35538530").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="35538530"><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="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="24009" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Star formation (Physics)</a>, <script data-card-contents-for-ri="24009" type="text/json">{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="70376" rel="nofollow" href="https://www.academia.edu/Documents/in/Massive_Star_Formation">Massive Star Formation</a>, <script data-card-contents-for-ri="70376" type="text/json">{"id":70376,"name":"Massive Star Formation","url":"https://www.academia.edu/Documents/in/Massive_Star_Formation?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="75789" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation">Interstellar Medium and Star formation</a><script data-card-contents-for-ri="75789" type="text/json">{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=24009","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=35538530]'), work: {"id":35538530,"title":"High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22","created_at":"2017-12-29T17:29:23.908-08:00","url":"https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22?f_ri=24009","dom_id":"work_35538530","summary":"How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 M e Myr −1 , suggesting the hub mass would be doubled in six free-fall times, adding up to ∼2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO + (3–2) and 13 CO(3–2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s −1 and 7.2×10 −4 M e yr −1 , respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11–15 M e and it is still growing with an accretion rate of 7×10 −5 M e yr −1. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.","downloadable_attachments":[{"id":55404248,"asset_id":35538530,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":66695878,"first_name":"Jinghua","last_name":"Yuan","domain_name":"gucas","page_name":"jhyuannaoc","display_name":"Jinghua Yuan","profile_url":"https://gucas.academia.edu/jhyuannaoc?f_ri=24009","photo":"https://0.academia-photos.com/66695878/17364443/17484885/s65_jinghua.yuan.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true},{"id":70376,"name":"Massive Star Formation","url":"https://www.academia.edu/Documents/in/Massive_Star_Formation?f_ri=24009","nofollow":true},{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=24009","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_32454247" data-work_id="32454247" 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/32454247/A_Magnetized_Jet_from_a_Massive_Protostar">A Magnetized Jet from a Massive Protostar</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Synchrotron emission is commonly found in relativistic jets from active galactic nuclei (AGNs) and microquasars, but so far its presence in jets from young stellar objects (YSOs) has not been proved. Here, we present evidence of polarized... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_32454247" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Synchrotron emission is commonly found in relativistic jets from active galactic nuclei (AGNs) and microquasars, but so far its presence in jets from young stellar objects (YSOs) has not been proved. Here, we present evidence of polarized synchrotron emission arising from the jet of a YSO. The apparent magnetic field, with strength of ∼0.2 milligauss, is parallel to the jet axis, and the polarization degree increases towards the jet edges, as expected for a confining helical magnetic field configuration. These characteristics are similar to those found in AGN jets, hinting at a common origin of all astrophysical jets. Supersonic jets are observed to emerge from a wide variety of astrophysical systems, from young brown dwarfs to active galatic nuclei (AGNs). Despite their different physical scales (from hundreds to billions of astronomical units), they have strong morphological similarites (1), and a common feature of these systems is the presence of a gaseous disk around the central object. However, it is yet unclear whether there is a universal mechanism that can explain the origin of all these jets.</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/32454247" 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="efb9a201254eb568db0f878682b251a7" rel="nofollow" data-download="{"attachment_id":52644333,"asset_id":32454247,"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/52644333/download_file?st=MTc0MDAzNDU3NCw4LjIyMi4yMDguMTQ2&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="63079494" href="https://independent.academia.edu/MayraOsorio6">Mayra Osorio</a><script data-card-contents-for-user="63079494" type="text/json">{"id":63079494,"first_name":"Mayra","last_name":"Osorio","domain_name":"independent","page_name":"MayraOsorio6","display_name":"Mayra Osorio","profile_url":"https://independent.academia.edu/MayraOsorio6?f_ri=24009","photo":"https://0.academia-photos.com/63079494/34618826/30353943/s65_mayra.osorio.jpg"}</script></span></span></li><li class="js-paper-rank-work_32454247 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="32454247"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 32454247, container: ".js-paper-rank-work_32454247", }); });</script></li><li class="js-percentile-work_32454247 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 = 32454247; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_32454247"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_32454247 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="32454247"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 32454247; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=32454247]").text(description); $(".js-view-count-work_32454247").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_32454247").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="32454247"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4742" rel="nofollow" href="https://www.academia.edu/Documents/in/Active_Galactic_Nuclei">Active Galactic Nuclei</a>, <script data-card-contents-for-ri="4742" type="text/json">{"id":4742,"name":"Active Galactic Nuclei","url":"https://www.academia.edu/Documents/in/Active_Galactic_Nuclei?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="6779" rel="nofollow" href="https://www.academia.edu/Documents/in/Science">Science</a>, <script data-card-contents-for-ri="6779" type="text/json">{"id":6779,"name":"Science","url":"https://www.academia.edu/Documents/in/Science?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="24009" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Star formation (Physics)</a>, <script data-card-contents-for-ri="24009" type="text/json">{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="28235" rel="nofollow" href="https://www.academia.edu/Documents/in/Multidisciplinary">Multidisciplinary</a><script data-card-contents-for-ri="28235" type="text/json">{"id":28235,"name":"Multidisciplinary","url":"https://www.academia.edu/Documents/in/Multidisciplinary?f_ri=24009","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=32454247]'), work: {"id":32454247,"title":"A Magnetized Jet from a Massive Protostar","created_at":"2017-04-17T02:53:23.769-07:00","url":"https://www.academia.edu/32454247/A_Magnetized_Jet_from_a_Massive_Protostar?f_ri=24009","dom_id":"work_32454247","summary":"Synchrotron emission is commonly found in relativistic jets from active galactic nuclei (AGNs) and microquasars, but so far its presence in jets from young stellar objects (YSOs) has not been proved. Here, we present evidence of polarized synchrotron emission arising from the jet of a YSO. The apparent magnetic field, with strength of ∼0.2 milligauss, is parallel to the jet axis, and the polarization degree increases towards the jet edges, as expected for a confining helical magnetic field configuration. These characteristics are similar to those found in AGN jets, hinting at a common origin of all astrophysical jets. Supersonic jets are observed to emerge from a wide variety of astrophysical systems, from young brown dwarfs to active galatic nuclei (AGNs). Despite their different physical scales (from hundreds to billions of astronomical units), they have strong morphological similarites (1), and a common feature of these systems is the presence of a gaseous disk around the central object. However, it is yet unclear whether there is a universal mechanism that can explain the origin of all these jets.","downloadable_attachments":[{"id":52644333,"asset_id":32454247,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":63079494,"first_name":"Mayra","last_name":"Osorio","domain_name":"independent","page_name":"MayraOsorio6","display_name":"Mayra Osorio","profile_url":"https://independent.academia.edu/MayraOsorio6?f_ri=24009","photo":"https://0.academia-photos.com/63079494/34618826/30353943/s65_mayra.osorio.jpg"}],"research_interests":[{"id":4742,"name":"Active Galactic Nuclei","url":"https://www.academia.edu/Documents/in/Active_Galactic_Nuclei?f_ri=24009","nofollow":true},{"id":6779,"name":"Science","url":"https://www.academia.edu/Documents/in/Science?f_ri=24009","nofollow":true},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true},{"id":28235,"name":"Multidisciplinary","url":"https://www.academia.edu/Documents/in/Multidisciplinary?f_ri=24009","nofollow":true},{"id":34754,"name":"Magnetic field","url":"https://www.academia.edu/Documents/in/Magnetic_field?f_ri=24009"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_24763208" data-work_id="24763208" 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/24763208/Search_for_a_Circumbinary_Disk_and_Accretion_Streams_onto_the_Circumstellar_Disks_of_the_Binary_Protostellar_System_L1551_IRS5">Search for a Circumbinary Disk and Accretion Streams onto the Circumstellar Disks of the Binary Protostellar System L1551 IRS5</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 formation of binary and multiple star systems are thought to be due to fragmen- tation of cores. The two main candidates for how this fragmentation occurs are bulk rotation and turbulence. These two models predict different alignments... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_24763208" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The formation of binary and multiple star systems are thought to be due to fragmen-<br />tation of cores. The two main candidates for how this fragmentation occurs are bulk<br />rotation and turbulence. These two models predict different alignments for the spins and<br />orbits of the stars and their circumstellar disks but due to internal and external pertur-<br />bations, the system can result in being either aligned or misaligned. This would hide<br />the details of how the system actually came to be. In this project, we have performed<br />data reduction and analysis on data pertaining to the binary protostellar system L1551<br />IRS5. The principal goal of our research was to look for a possible circumbinary disk<br />around the binary components, as well as to search for structures that extend from the<br />circumstellar disks which would correlate to matter infall and accretion streams.<br />The observations were made using the B and C Arrays of the Very Large Array<br />(VLA). The search for the circumbinary disk was done using the C array observations,<br />since this provides lower angular resolutions which correspond to large angular scales.<br />This enabled us to look for structures spanning larger scales, which is what is expected<br />of a circumbinary disk. The B array observations were used to search for the structures<br />extending from the circumstellar disks, since this provides high angular resolution at<br />small angular scales. This allowed us to look into the structure in detail so as to study<br />the accretion streams. As the final product, we created images as well as a residual map<br />from one dataset and found that there were certain distinctive structures surrounding<br />the circumstellar disks which may correspond to possible accretion streams. The cir-<br />cumbinary disk was not detected as of yet which may be due to insufficient angular scale<br />in the observations. However our residual maps are based on basic model-subtraction<br />of only the circumstellar disks. Model-subtraction with higher accuracy will be carried<br />out on all datasets in the future to obtain the residual images which will provide better<br />insight into the nature of the structures protruding from the circumstellar disks.</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/24763208" 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="4c43152e01e56156aed18b258e928a8f" rel="nofollow" data-download="{"attachment_id":45092848,"asset_id":24763208,"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/45092848/download_file?st=MTc0MDAzNDU3NCw4LjIyMi4yMDguMTQ2&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="12863366" href="https://hku-hk.academia.edu/AmruthAlfred">Amruth Alfred</a><script data-card-contents-for-user="12863366" type="text/json">{"id":12863366,"first_name":"Amruth","last_name":"Alfred","domain_name":"hku-hk","page_name":"AmruthAlfred","display_name":"Amruth Alfred","profile_url":"https://hku-hk.academia.edu/AmruthAlfred?f_ri=24009","photo":"https://0.academia-photos.com/12863366/5386665/6148301/s65_amruth.alfred.jpg_oh_7c8991e9d6eed2e33f2e29eb823b978b_oe_54f72bb0___gda___1425078216_357620164ece576bbb5e46a8bac04025"}</script></span></span></li><li class="js-paper-rank-work_24763208 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="24763208"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 24763208, container: ".js-paper-rank-work_24763208", }); });</script></li><li class="js-percentile-work_24763208 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 = 24763208; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_24763208"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_24763208 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="24763208"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 24763208; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=24763208]").text(description); $(".js-view-count-work_24763208").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_24763208").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="24763208"><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="498" rel="nofollow" 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=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="701" rel="nofollow" href="https://www.academia.edu/Documents/in/Radio_Astronomy">Radio Astronomy</a>, <script data-card-contents-for-ri="701" type="text/json">{"id":701,"name":"Radio Astronomy","url":"https://www.academia.edu/Documents/in/Radio_Astronomy?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" rel="nofollow" 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=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="24009" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Star formation (Physics)</a><script data-card-contents-for-ri="24009" type="text/json">{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=24763208]'), work: {"id":24763208,"title":"Search for a Circumbinary Disk and Accretion Streams onto the Circumstellar Disks of the Binary Protostellar System L1551 IRS5","created_at":"2016-04-26T02:44:19.273-07:00","url":"https://www.academia.edu/24763208/Search_for_a_Circumbinary_Disk_and_Accretion_Streams_onto_the_Circumstellar_Disks_of_the_Binary_Protostellar_System_L1551_IRS5?f_ri=24009","dom_id":"work_24763208","summary":"The formation of binary and multiple star systems are thought to be due to fragmen-\ntation of cores. The two main candidates for how this fragmentation occurs are bulk\nrotation and turbulence. These two models predict different alignments for the spins and\norbits of the stars and their circumstellar disks but due to internal and external pertur-\nbations, the system can result in being either aligned or misaligned. This would hide\nthe details of how the system actually came to be. In this project, we have performed\ndata reduction and analysis on data pertaining to the binary protostellar system L1551\nIRS5. The principal goal of our research was to look for a possible circumbinary disk\naround the binary components, as well as to search for structures that extend from the\ncircumstellar disks which would correlate to matter infall and accretion streams.\nThe observations were made using the B and C Arrays of the Very Large Array\n(VLA). The search for the circumbinary disk was done using the C array observations,\nsince this provides lower angular resolutions which correspond to large angular scales.\nThis enabled us to look for structures spanning larger scales, which is what is expected\nof a circumbinary disk. The B array observations were used to search for the structures\nextending from the circumstellar disks, since this provides high angular resolution at\nsmall angular scales. This allowed us to look into the structure in detail so as to study\nthe accretion streams. As the final product, we created images as well as a residual map\nfrom one dataset and found that there were certain distinctive structures surrounding\nthe circumstellar disks which may correspond to possible accretion streams. The cir-\ncumbinary disk was not detected as of yet which may be due to insufficient angular scale\nin the observations. However our residual maps are based on basic model-subtraction\nof only the circumstellar disks. Model-subtraction with higher accuracy will be carried\nout on all datasets in the future to obtain the residual images which will provide better\ninsight into the nature of the structures protruding from the circumstellar disks.","downloadable_attachments":[{"id":45092848,"asset_id":24763208,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":12863366,"first_name":"Amruth","last_name":"Alfred","domain_name":"hku-hk","page_name":"AmruthAlfred","display_name":"Amruth Alfred","profile_url":"https://hku-hk.academia.edu/AmruthAlfred?f_ri=24009","photo":"https://0.academia-photos.com/12863366/5386665/6148301/s65_amruth.alfred.jpg_oh_7c8991e9d6eed2e33f2e29eb823b978b_oe_54f72bb0___gda___1425078216_357620164ece576bbb5e46a8bac04025"}],"research_interests":[{"id":498,"name":"Physics","url":"https://www.academia.edu/Documents/in/Physics?f_ri=24009","nofollow":true},{"id":701,"name":"Radio Astronomy","url":"https://www.academia.edu/Documents/in/Radio_Astronomy?f_ri=24009","nofollow":true},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=24009","nofollow":true},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=24009"},{"id":58143,"name":"Interferometry","url":"https://www.academia.edu/Documents/in/Interferometry?f_ri=24009"},{"id":1709249,"name":"Very Large Array","url":"https://www.academia.edu/Documents/in/Very_Large_Array?f_ri=24009"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_339239" data-work_id="339239" 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/339239/The_Star_Formation_Rate_and_Gas_Surface_Density_Relation_In_the_Milky_Way_Implications_for_Extragalactic_Studies">The Star Formation Rate and Gas Surface Density Relation In the Milky Way: Implications for Extragalactic Studies</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/339239" 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="af2a72eb699479de4caa3a55f4bff700" rel="nofollow" data-download="{"attachment_id":1728812,"asset_id":339239,"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/1728812/download_file?st=MTc0MDAzNDU3NCw4LjIyMi4yMDguMTQ2&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="157219" href="https://utexas.academia.edu/AmandaHeiderman">Amanda Heiderman</a><script data-card-contents-for-user="157219" type="text/json">{"id":157219,"first_name":"Amanda","last_name":"Heiderman","domain_name":"utexas","page_name":"AmandaHeiderman","display_name":"Amanda Heiderman","profile_url":"https://utexas.academia.edu/AmandaHeiderman?f_ri=24009","photo":"https://0.academia-photos.com/157219/40642/37352/s65_amanda.heiderman.jpg"}</script></span></span></li><li class="js-paper-rank-work_339239 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="339239"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 339239, container: ".js-paper-rank-work_339239", }); });</script></li><li class="js-percentile-work_339239 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 = 339239; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_339239"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_339239 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="339239"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 339239; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=339239]").text(description); $(".js-view-count-work_339239").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_339239").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="339239"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11049" rel="nofollow" href="https://www.academia.edu/Documents/in/Extragalactic_Astronomy">Extragalactic Astronomy</a>, <script data-card-contents-for-ri="11049" type="text/json">{"id":11049,"name":"Extragalactic Astronomy","url":"https://www.academia.edu/Documents/in/Extragalactic_Astronomy?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="24009" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Star formation (Physics)</a>, <script data-card-contents-for-ri="24009" type="text/json">{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="162318" rel="nofollow" href="https://www.academia.edu/Documents/in/Extragalactic_Star_Formation">Extragalactic Star Formation</a><script data-card-contents-for-ri="162318" type="text/json">{"id":162318,"name":"Extragalactic Star Formation","url":"https://www.academia.edu/Documents/in/Extragalactic_Star_Formation?f_ri=24009","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=339239]'), work: {"id":339239,"title":"The Star Formation Rate and Gas Surface Density Relation In the Milky Way: Implications for Extragalactic Studies","created_at":"2010-09-25T19:08:49.640-07:00","url":"https://www.academia.edu/339239/The_Star_Formation_Rate_and_Gas_Surface_Density_Relation_In_the_Milky_Way_Implications_for_Extragalactic_Studies?f_ri=24009","dom_id":"work_339239","summary":null,"downloadable_attachments":[{"id":1728812,"asset_id":339239,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":157219,"first_name":"Amanda","last_name":"Heiderman","domain_name":"utexas","page_name":"AmandaHeiderman","display_name":"Amanda Heiderman","profile_url":"https://utexas.academia.edu/AmandaHeiderman?f_ri=24009","photo":"https://0.academia-photos.com/157219/40642/37352/s65_amanda.heiderman.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true},{"id":11049,"name":"Extragalactic Astronomy","url":"https://www.academia.edu/Documents/in/Extragalactic_Astronomy?f_ri=24009","nofollow":true},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true},{"id":162318,"name":"Extragalactic Star Formation","url":"https://www.academia.edu/Documents/in/Extragalactic_Star_Formation?f_ri=24009","nofollow":true},{"id":162319,"name":"Milky Way","url":"https://www.academia.edu/Documents/in/Milky_Way?f_ri=24009"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_59983134" data-work_id="59983134" 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/59983134/Deuterium_and_15N_fractionation_in_N2H_during_the_formation_of_a_Sun_like_star">Deuterium and 15N fractionation in N2H+ during the formation of a Sun-like 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">Although chemical models predict that the deuterium fractionation in N 2 H + is a good evolutionary tracer in the star formation process, the fractionation of nitrogen is still a poorly understood process. Recent models have questioned... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_59983134" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Although chemical models predict that the deuterium fractionation in N 2 H + is a good evolutionary tracer in the star formation process, the fractionation of nitrogen is still a poorly understood process. Recent models have questioned the similar evolutionary trend expected for the two fractionation mechanisms in N 2 H + , based on a classical scenario in which ionneutral reactions occurring in cold gas should have caused an enhancement of the abundance of N 2 D + , 15 NNH + , and N 15 NH +. In the framework of the ASAI IRAM-30m large program, we have investigated the fractionation of deuterium and 15 N in N 2 H + in the best known representatives of the different evolutionary stages of the Sun-like star formation process. The goal is to ultimately confirm (or deny) the classical 'ion-neutral reactions' scenario that predicts a similar trend for D and 15 N fractionation. We do not find any evolutionary trend of the 14 N/ 15 N ratio from both the 15 NNH + and N 15 NH + isotopologues. Therefore, our findings confirm that, during the formation of a Sun-like star, the core evolution is irrelevant in the fractionation of 15 N. The independence of the 14 N/ 15 N ratio with time, found also in high-mass star-forming cores, indicates that the enrichment in 15 N revealed in comets and protoplanetary discs is unlikely to happen at core scales. Nevertheless, we have firmly confirmed the evolutionary trend expected for the H/D ratio, with the N 2 H + /N 2 D + ratio decreasing before the pre-stellar core phase, and increasing monotonically during the protostellar phase. We have also confirmed clearly that the two fractionation mechanisms are not related.</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/59983134" 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="aeb4b11d82c4ec280451399be894514e" rel="nofollow" data-download="{"attachment_id":73631286,"asset_id":59983134,"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/73631286/download_file?st=MTc0MDAzNDU3NCw4LjIyMi4yMDguMTQ2&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="35241180" href="https://independent.academia.edu/ECaux">E. Caux</a><script data-card-contents-for-user="35241180" type="text/json">{"id":35241180,"first_name":"E.","last_name":"Caux","domain_name":"independent","page_name":"ECaux","display_name":"E. Caux","profile_url":"https://independent.academia.edu/ECaux?f_ri=24009","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_59983134 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="59983134"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 59983134, container: ".js-paper-rank-work_59983134", }); });</script></li><li class="js-percentile-work_59983134 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 = 59983134; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_59983134"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_59983134 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="59983134"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 59983134; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=59983134]").text(description); $(".js-view-count-work_59983134").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_59983134").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="59983134"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11124" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrochemistry">Astrochemistry</a>, <script data-card-contents-for-ri="11124" type="text/json">{"id":11124,"name":"Astrochemistry","url":"https://www.academia.edu/Documents/in/Astrochemistry?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="24009" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Star formation (Physics)</a>, <script data-card-contents-for-ri="24009" type="text/json">{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="75789" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation">Interstellar Medium and Star formation</a><script data-card-contents-for-ri="75789" type="text/json">{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=24009","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=59983134]'), work: {"id":59983134,"title":"Deuterium and 15N fractionation in N2H+ during the formation of a Sun-like star","created_at":"2021-10-25T22:57:27.309-07:00","url":"https://www.academia.edu/59983134/Deuterium_and_15N_fractionation_in_N2H_during_the_formation_of_a_Sun_like_star?f_ri=24009","dom_id":"work_59983134","summary":"Although chemical models predict that the deuterium fractionation in N 2 H + is a good evolutionary tracer in the star formation process, the fractionation of nitrogen is still a poorly understood process. Recent models have questioned the similar evolutionary trend expected for the two fractionation mechanisms in N 2 H + , based on a classical scenario in which ionneutral reactions occurring in cold gas should have caused an enhancement of the abundance of N 2 D + , 15 NNH + , and N 15 NH +. In the framework of the ASAI IRAM-30m large program, we have investigated the fractionation of deuterium and 15 N in N 2 H + in the best known representatives of the different evolutionary stages of the Sun-like star formation process. The goal is to ultimately confirm (or deny) the classical 'ion-neutral reactions' scenario that predicts a similar trend for D and 15 N fractionation. We do not find any evolutionary trend of the 14 N/ 15 N ratio from both the 15 NNH + and N 15 NH + isotopologues. Therefore, our findings confirm that, during the formation of a Sun-like star, the core evolution is irrelevant in the fractionation of 15 N. The independence of the 14 N/ 15 N ratio with time, found also in high-mass star-forming cores, indicates that the enrichment in 15 N revealed in comets and protoplanetary discs is unlikely to happen at core scales. Nevertheless, we have firmly confirmed the evolutionary trend expected for the H/D ratio, with the N 2 H + /N 2 D + ratio decreasing before the pre-stellar core phase, and increasing monotonically during the protostellar phase. We have also confirmed clearly that the two fractionation mechanisms are not related.","downloadable_attachments":[{"id":73631286,"asset_id":59983134,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":35241180,"first_name":"E.","last_name":"Caux","domain_name":"independent","page_name":"ECaux","display_name":"E. Caux","profile_url":"https://independent.academia.edu/ECaux?f_ri=24009","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true},{"id":11124,"name":"Astrochemistry","url":"https://www.academia.edu/Documents/in/Astrochemistry?f_ri=24009","nofollow":true},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true},{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=24009","nofollow":true},{"id":526952,"name":"Fractionation","url":"https://www.academia.edu/Documents/in/Fractionation?f_ri=24009"},{"id":535357,"name":"Low Mass Stars","url":"https://www.academia.edu/Documents/in/Low_Mass_Stars?f_ri=24009"},{"id":640682,"name":"Isotope fractionation","url":"https://www.academia.edu/Documents/in/Isotope_fractionation?f_ri=24009"},{"id":1229679,"name":"Isotopologues","url":"https://www.academia.edu/Documents/in/Isotopologues?f_ri=24009"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_30189441 coauthored" data-work_id="30189441" 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/30189441/Protostellar_Outflows_in_L1340">Protostellar Outflows in L1340</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 have searched the L1340 A, B, and C clouds for shocks from protostellar outflows using the H 2 2.122 µm near-IR line as a shock tracer. Substantial out-flow activity has been found in each of the three regions of the cloud (L1340 A,... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_30189441" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We have searched the L1340 A, B, and C clouds for shocks from protostellar outflows using the H 2 2.122 µm near-IR line as a shock tracer. Substantial out-flow activity has been found in each of the three regions of the cloud (L1340 A, L1340 B, & L1340 C). We find 42 distinct shock complexes (16 in L1340 A, 11 in L1340 B, and 15 in L1340 C). We were able to link 17 of those shock complexes in to 12 distinct outflows and identify candidate source stars for each. We examine the properties (A V , T bol , and L bol) of the source protostars and compare that to the properties of the general population of Class 0/I and flat SED protostars and find that there is an indication, albeit at low statistical significance, that the outflow driving protostars are drawn from a population with lower A V , higher L bol , and lower T bol than the general population of protostars.</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/30189441" 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="67878006916c4c4d3fc3d6c366be2155" rel="nofollow" data-download="{"attachment_id":50648735,"asset_id":30189441,"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/50648735/download_file?st=MTc0MDAzNDU3NCw4LjIyMi4yMDguMTQ2&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="1575479" href="https://caltech.academia.edu/JoAnnOLinger">JoAnn O'Linger</a><script data-card-contents-for-user="1575479" type="text/json">{"id":1575479,"first_name":"JoAnn","last_name":"O'Linger","domain_name":"caltech","page_name":"JoAnnOLinger","display_name":"JoAnn O'Linger","profile_url":"https://caltech.academia.edu/JoAnnOLinger?f_ri=24009","photo":"https://0.academia-photos.com/1575479/552936/15306751/s65_joann.o_linger.jpg"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-30189441">+2</span><div class="hidden js-additional-users-30189441"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://adlerplanetarium.academia.edu/GraceWolfChase">Grace Wolf-Chase</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://northwestern.academia.edu/MichaelSmutko">Michael Smutko</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-30189441'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-30189441').html(); } } new HoverPopover(popoverSettings); })();</script></li><li class="js-paper-rank-work_30189441 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="30189441"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 30189441, container: ".js-paper-rank-work_30189441", }); });</script></li><li class="js-percentile-work_30189441 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 = 30189441; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_30189441"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_30189441 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="30189441"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 30189441; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=30189441]").text(description); $(".js-view-count-work_30189441").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_30189441").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="30189441"><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="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="24009" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Star formation (Physics)</a>, <script data-card-contents-for-ri="24009" type="text/json">{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="75789" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation">Interstellar Medium and Star formation</a>, <script data-card-contents-for-ri="75789" type="text/json">{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1131724" rel="nofollow" href="https://www.academia.edu/Documents/in/Protostellar_Outflows">Protostellar Outflows</a><script data-card-contents-for-ri="1131724" type="text/json">{"id":1131724,"name":"Protostellar Outflows","url":"https://www.academia.edu/Documents/in/Protostellar_Outflows?f_ri=24009","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=30189441]'), work: {"id":30189441,"title":"Protostellar Outflows in L1340","created_at":"2016-11-30T20:04:19.146-08:00","url":"https://www.academia.edu/30189441/Protostellar_Outflows_in_L1340?f_ri=24009","dom_id":"work_30189441","summary":"We have searched the L1340 A, B, and C clouds for shocks from protostellar outflows using the H 2 2.122 µm near-IR line as a shock tracer. Substantial out-flow activity has been found in each of the three regions of the cloud (L1340 A, L1340 B, \u0026 L1340 C). We find 42 distinct shock complexes (16 in L1340 A, 11 in L1340 B, and 15 in L1340 C). We were able to link 17 of those shock complexes in to 12 distinct outflows and identify candidate source stars for each. We examine the properties (A V , T bol , and L bol) of the source protostars and compare that to the properties of the general population of Class 0/I and flat SED protostars and find that there is an indication, albeit at low statistical significance, that the outflow driving protostars are drawn from a population with lower A V , higher L bol , and lower T bol than the general population of protostars.","downloadable_attachments":[{"id":50648735,"asset_id":30189441,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":1575479,"first_name":"JoAnn","last_name":"O'Linger","domain_name":"caltech","page_name":"JoAnnOLinger","display_name":"JoAnn O'Linger","profile_url":"https://caltech.academia.edu/JoAnnOLinger?f_ri=24009","photo":"https://0.academia-photos.com/1575479/552936/15306751/s65_joann.o_linger.jpg"},{"id":2235051,"first_name":"Grace","last_name":"Wolf-Chase","domain_name":"adlerplanetarium","page_name":"GraceWolfChase","display_name":"Grace Wolf-Chase","profile_url":"https://adlerplanetarium.academia.edu/GraceWolfChase?f_ri=24009","photo":"/images/s65_no_pic.png"},{"id":54658842,"first_name":"Michael","last_name":"Smutko","domain_name":"northwestern","page_name":"MichaelSmutko","display_name":"Michael Smutko","profile_url":"https://northwestern.academia.edu/MichaelSmutko?f_ri=24009","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009","nofollow":true},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009","nofollow":true},{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=24009","nofollow":true},{"id":1131724,"name":"Protostellar Outflows","url":"https://www.academia.edu/Documents/in/Protostellar_Outflows?f_ri=24009","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_34503486" data-work_id="34503486" 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/34503486/The_Problems_with_the_Notion_of_Black_Holes">The Problems with the Notion of Black Holes</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 problems with the notion of black holes are numerous, but I'll go through a few of the main ones. Black Holes as the core of spiral galaxies: When we look at pictures of spiral galaxies, intuitively we're reminded of whirlpools or the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_34503486" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The problems with the notion of black holes are numerous, but I'll go through a few of the main ones. Black Holes as the core of spiral galaxies: When we look at pictures of spiral galaxies, intuitively we're reminded of whirlpools or the gaseous equivalents, such as tornadoes or dust devils. That intuition leads us to see the 'arms' of the spiral as 'trailing', which implies that the galaxy, in the same sense as a whirlpool, is 'pulling' matter in to it. The solar system is posited as being, currently, towards the end of one such 'trailing' arm. The problem with this intuition is that whirlpools and equivalents can only form where the 'forces' of things surrounding them are greater than the forces generated by the whirlpool itself. In the case of a galaxy, where there is very little between it and the next galaxy, that's problematic. Granted there is such a thing as 'dark matter' and 'dark energy', it would have to be fairly evenly distributed both within and without the galaxy, otherwise it would be detectable and not 'dark', that distribution means that it can't change the overall sense that there's very little between galaxies, it just adds the qualifier 'very little that has any effective capacity " between galaxies. Observationally, this difference and therefore the intuition that ignores it, are incorrect. The spin of spiral galaxies, insofar as it can be determined (spiral galaxies spin at very different rates, which makes the direction of the spin difficult to determine in cases where the rate is relatively slow) is inverse to the intuitive spin, meaning the 'arms' of the spiral are actually leading arms, not trailing arms. Simultaneously this implies that the galaxy is not 'pulling' anything from its surrounding region, but pushing into its surrounding region. For a galaxy to endure for any length of time, therefore, the galaxy must be producing, rather than consuming, matter and energy in some way. This also fits with the observation that spiral galaxies, unlike other types which appear to be older, tend to be more isolated, further from the dense clusters of other types of galaxies. Were they to exist fundamentally by pulling things in from the surrounding area, one would expect them to be more prevalent where there was more in the surrounding area to draw in. Leaving aside the unanswered question of what the 'arms' actually consist of (the intuition that they consist of denser areas of stars is also incorrect – the orbits of stars around the galactic core are extremely eccentric in general, and don't correspond to the 'arms' in any way, thus in a few hundred thousand years, the sun is predicted to be much closer to the galactic core, but outside any of the arms –</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/34503486" 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="554ed8e80a2d14ae8bad972d04ffc604" rel="nofollow" data-download="{"attachment_id":54368314,"asset_id":34503486,"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/54368314/download_file?st=MTc0MDAzNDU3NCw4LjIyMi4yMDguMTQ2&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="173718" href="https://independent.academia.edu/AndrewGlynn">Andrew Glynn</a><script data-card-contents-for-user="173718" type="text/json">{"id":173718,"first_name":"Andrew","last_name":"Glynn","domain_name":"independent","page_name":"AndrewGlynn","display_name":"Andrew Glynn","profile_url":"https://independent.academia.edu/AndrewGlynn?f_ri=24009","photo":"https://0.academia-photos.com/173718/43432/39942/s65_andrew.glynn.jpg"}</script></span></span></li><li class="js-paper-rank-work_34503486 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="34503486"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 34503486, container: ".js-paper-rank-work_34503486", }); 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$(".js-view-count[data-work-id=34503486]").text(description); $(".js-view-count-work_34503486").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_34503486").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="34503486"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">9</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="518" rel="nofollow" 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=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="888" rel="nofollow" href="https://www.academia.edu/Documents/in/Cosmology_Physics_">Cosmology (Physics)</a>, <script data-card-contents-for-ri="888" type="text/json">{"id":888,"name":"Cosmology (Physics)","url":"https://www.academia.edu/Documents/in/Cosmology_Physics_?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1246" rel="nofollow" href="https://www.academia.edu/Documents/in/Gravitation">Gravitation</a>, <script data-card-contents-for-ri="1246" type="text/json">{"id":1246,"name":"Gravitation","url":"https://www.academia.edu/Documents/in/Gravitation?f_ri=24009","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2578" rel="nofollow" href="https://www.academia.edu/Documents/in/Particle_Physics">Particle Physics</a><script data-card-contents-for-ri="2578" type="text/json">{"id":2578,"name":"Particle Physics","url":"https://www.academia.edu/Documents/in/Particle_Physics?f_ri=24009","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=34503486]'), work: {"id":34503486,"title":"The Problems with the Notion of Black Holes","created_at":"2017-09-07T07:30:22.565-07:00","url":"https://www.academia.edu/34503486/The_Problems_with_the_Notion_of_Black_Holes?f_ri=24009","dom_id":"work_34503486","summary":"The problems with the notion of black holes are numerous, but I'll go through a few of the main ones. Black Holes as the core of spiral galaxies: When we look at pictures of spiral galaxies, intuitively we're reminded of whirlpools or the gaseous equivalents, such as tornadoes or dust devils. That intuition leads us to see the 'arms' of the spiral as 'trailing', which implies that the galaxy, in the same sense as a whirlpool, is 'pulling' matter in to it. The solar system is posited as being, currently, towards the end of one such 'trailing' arm. The problem with this intuition is that whirlpools and equivalents can only form where the 'forces' of things surrounding them are greater than the forces generated by the whirlpool itself. In the case of a galaxy, where there is very little between it and the next galaxy, that's problematic. Granted there is such a thing as 'dark matter' and 'dark energy', it would have to be fairly evenly distributed both within and without the galaxy, otherwise it would be detectable and not 'dark', that distribution means that it can't change the overall sense that there's very little between galaxies, it just adds the qualifier 'very little that has any effective capacity \" between galaxies. Observationally, this difference and therefore the intuition that ignores it, are incorrect. The spin of spiral galaxies, insofar as it can be determined (spiral galaxies spin at very different rates, which makes the direction of the spin difficult to determine in cases where the rate is relatively slow) is inverse to the intuitive spin, meaning the 'arms' of the spiral are actually leading arms, not trailing arms. Simultaneously this implies that the galaxy is not 'pulling' anything from its surrounding region, but pushing into its surrounding region. For a galaxy to endure for any length of time, therefore, the galaxy must be producing, rather than consuming, matter and energy in some way. This also fits with the observation that spiral galaxies, unlike other types which appear to be older, tend to be more isolated, further from the dense clusters of other types of galaxies. Were they to exist fundamentally by pulling things in from the surrounding area, one would expect them to be more prevalent where there was more in the surrounding area to draw in. Leaving aside the unanswered question of what the 'arms' actually consist of (the intuition that they consist of denser areas of stars is also incorrect – the orbits of stars around the galactic core are extremely eccentric in general, and don't correspond to the 'arms' in any way, thus in a few hundred thousand years, the sun is predicted to be much closer to the galactic core, but outside any of the arms –","downloadable_attachments":[{"id":54368314,"asset_id":34503486,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":173718,"first_name":"Andrew","last_name":"Glynn","domain_name":"independent","page_name":"AndrewGlynn","display_name":"Andrew Glynn","profile_url":"https://independent.academia.edu/AndrewGlynn?f_ri=24009","photo":"https://0.academia-photos.com/173718/43432/39942/s65_andrew.glynn.jpg"}],"research_interests":[{"id":518,"name":"Quantum Physics","url":"https://www.academia.edu/Documents/in/Quantum_Physics?f_ri=24009","nofollow":true},{"id":888,"name":"Cosmology (Physics)","url":"https://www.academia.edu/Documents/in/Cosmology_Physics_?f_ri=24009","nofollow":true},{"id":1246,"name":"Gravitation","url":"https://www.academia.edu/Documents/in/Gravitation?f_ri=24009","nofollow":true},{"id":2578,"name":"Particle Physics","url":"https://www.academia.edu/Documents/in/Particle_Physics?f_ri=24009","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=24009"},{"id":4751,"name":"Black Holes","url":"https://www.academia.edu/Documents/in/Black_Holes?f_ri=24009"},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=24009"},{"id":51564,"name":"Stephen Hawking","url":"https://www.academia.edu/Documents/in/Stephen_Hawking?f_ri=24009"},{"id":584714,"name":"Event horizon","url":"https://www.academia.edu/Documents/in/Event_horizon?f_ri=24009"}]}, }) } })();</script></ul></li></ul></div></div></div><div class="u-taCenter Pagination"><ul class="pagination"></ul></div></div><div class="hidden-xs hidden-sm"><div class="u-pl6x"><div style="width: 300px;"><div class="panel panel-flat u-mt7x"><div class="panel-heading u-p5x"><div class="u-tcGrayDark u-taCenter u-fw700 u-textUppercase">Related Topics</div></div><ul class="list-group"><li class="list-group-item media_v2 u-mt0x u-p3x"><div class="media-body"><div class="u-tcGrayDarker u-fw700"><a class="u-tcGrayDarker" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a></div></div><div class="media-right media-middle"><a class="u-tcGreen u-textDecorationNone u-linkUnstyled u-fw500 hidden" data-follow-ri-id="4363">Follow</a><a class="u-tcGray u-textDecorationNone u-linkUnstyled u-fw500 hidden" data-unfollow-ri-id="4363">Following</a></div></li><li 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