On monolithic supermassive stars
ABSTRACT Supermassive stars have been proposed as the progenitors of the massive ($\sim \!10^{9}\, \mathrm{M}_{\odot }$) quasars observed at z ∼ 7. Prospects for directly detecting supermassive stars with next-generation facilities depend critically on their intrinsic lifetimes, as well as their for...
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creator | Woods, Tyrone E Heger, Alexander Haemmerlé, Lionel |
description | ABSTRACT
Supermassive stars have been proposed as the progenitors of the massive ($\sim \!10^{9}\, \mathrm{M}_{\odot }$) quasars observed at z ∼ 7. Prospects for directly detecting supermassive stars with next-generation facilities depend critically on their intrinsic lifetimes, as well as their formation rates. We use the one-dimensional stellar evolution code kepler to explore the theoretical limiting case of zero-metallicity non-rotating stars, formed monolithically with initial masses between $10$ and $190\, \mathrm{kM}_{\odot }$. We find that stars born with masses between $\sim\! 60$ and $\sim\! 150\, \mathrm{kM}_{\odot }$ collapse at the end of the main sequence, burning stably for $\sim\! 1.5\, \mathrm{Myr}$. More massive stars collapse directly through the general relativistic instability after only a thermal time-scale of $\sim\! 3$–$4\, \mathrm{kyr}$. The expected difficulty in producing such massive thermally relaxed objects, together with recent results for currently preferred rapidly accreting formation models, suggests that such ‘truly direct’ or ‘dark’ collapses may not be typical for supermassive objects in the early Universe. We close by discussing the evolution of supermassive stars in the broader context of massive primordial stellar evolution and the possibility of supermassive stellar explosions. |
doi_str_mv | 10.1093/mnras/staa763 |
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Supermassive stars have been proposed as the progenitors of the massive ($\sim \!10^{9}\, \mathrm{M}_{\odot }$) quasars observed at z ∼ 7. Prospects for directly detecting supermassive stars with next-generation facilities depend critically on their intrinsic lifetimes, as well as their formation rates. We use the one-dimensional stellar evolution code kepler to explore the theoretical limiting case of zero-metallicity non-rotating stars, formed monolithically with initial masses between $10$ and $190\, \mathrm{kM}_{\odot }$. We find that stars born with masses between $\sim\! 60$ and $\sim\! 150\, \mathrm{kM}_{\odot }$ collapse at the end of the main sequence, burning stably for $\sim\! 1.5\, \mathrm{Myr}$. More massive stars collapse directly through the general relativistic instability after only a thermal time-scale of $\sim\! 3$–$4\, \mathrm{kyr}$. The expected difficulty in producing such massive thermally relaxed objects, together with recent results for currently preferred rapidly accreting formation models, suggests that such ‘truly direct’ or ‘dark’ collapses may not be typical for supermassive objects in the early Universe. We close by discussing the evolution of supermassive stars in the broader context of massive primordial stellar evolution and the possibility of supermassive stellar explosions.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/staa763</identifier><language>eng</language><publisher>OXFORD: Oxford University Press</publisher><subject>Astronomy & Astrophysics ; Physical Sciences ; Science & Technology</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2020-05, Vol.494 (2), p.2236-2243</ispartof><rights>2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2020</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>true</woscitedreferencessubscribed><woscitedreferencescount>24</woscitedreferencescount><woscitedreferencesoriginalsourcerecordid>wos000535877200054</woscitedreferencesoriginalsourcerecordid><citedby>FETCH-LOGICAL-c336t-45f9edfda11a602fadd0a3d5ff70429bd4f7a53752ef5e9410495cd40553bfcc3</citedby><cites>FETCH-LOGICAL-c336t-45f9edfda11a602fadd0a3d5ff70429bd4f7a53752ef5e9410495cd40553bfcc3</cites><orcidid>0000-0002-3684-1325 ; 0000-0003-1428-5775</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>315,782,786,1586,1606,27931,27932,28255</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/staa763$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Woods, Tyrone E</creatorcontrib><creatorcontrib>Heger, Alexander</creatorcontrib><creatorcontrib>Haemmerlé, Lionel</creatorcontrib><title>On monolithic supermassive stars</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>MON NOT R ASTRON SOC</addtitle><description>ABSTRACT
Supermassive stars have been proposed as the progenitors of the massive ($\sim \!10^{9}\, \mathrm{M}_{\odot }$) quasars observed at z ∼ 7. Prospects for directly detecting supermassive stars with next-generation facilities depend critically on their intrinsic lifetimes, as well as their formation rates. We use the one-dimensional stellar evolution code kepler to explore the theoretical limiting case of zero-metallicity non-rotating stars, formed monolithically with initial masses between $10$ and $190\, \mathrm{kM}_{\odot }$. We find that stars born with masses between $\sim\! 60$ and $\sim\! 150\, \mathrm{kM}_{\odot }$ collapse at the end of the main sequence, burning stably for $\sim\! 1.5\, \mathrm{Myr}$. More massive stars collapse directly through the general relativistic instability after only a thermal time-scale of $\sim\! 3$–$4\, \mathrm{kyr}$. The expected difficulty in producing such massive thermally relaxed objects, together with recent results for currently preferred rapidly accreting formation models, suggests that such ‘truly direct’ or ‘dark’ collapses may not be typical for supermassive objects in the early Universe. We close by discussing the evolution of supermassive stars in the broader context of massive primordial stellar evolution and the possibility of supermassive stellar explosions.</description><subject>Astronomy & Astrophysics</subject><subject>Physical Sciences</subject><subject>Science & Technology</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>AOWDO</sourceid><recordid>eNqNj0tLxDAUhYMoWEeX7rsUJM5N82qXUnQUBmaj65LmgZFpU5JW8d_bsYNbXd2z-M7hfghdE7gjUNF110eV1mlUSgp6gjJCBcdFJcQpygAox6Uk5BxdpPQOAIwWIkP5rs-70Ie9H9-8ztM02NiplPyHzeelmC7RmVP7ZK-Od4VeHx9e6ie83W2e6_st1pSKETPuKmucUYQoAYVTxoCihjsngRVVa5iTilPJC-u4rRgBVnFtGHBOW6c1XSG87OoYUorWNUP0nYpfDYHmoNf86DVHvZkvF_7TtsEl7W2v7W9n9uOUl1IWh8RqP6rRh74OUz_O1dv_V2f6ZqHDNPzx0zejKnQ4</recordid><startdate>20200511</startdate><enddate>20200511</enddate><creator>Woods, Tyrone E</creator><creator>Heger, Alexander</creator><creator>Haemmerlé, Lionel</creator><general>Oxford University Press</general><general>Oxford Univ Press</general><scope>AOWDO</scope><scope>BLEPL</scope><scope>DTL</scope><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0002-3684-1325</orcidid><orcidid>https://orcid.org/0000-0003-1428-5775</orcidid></search><sort><creationdate>20200511</creationdate><title>On monolithic supermassive stars</title><author>Woods, Tyrone E ; Heger, Alexander ; Haemmerlé, Lionel</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c336t-45f9edfda11a602fadd0a3d5ff70429bd4f7a53752ef5e9410495cd40553bfcc3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Astronomy & Astrophysics</topic><topic>Physical Sciences</topic><topic>Science & Technology</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Woods, Tyrone E</creatorcontrib><creatorcontrib>Heger, Alexander</creatorcontrib><creatorcontrib>Haemmerlé, Lionel</creatorcontrib><collection>Web of Science - Science Citation Index Expanded - 2020</collection><collection>Web of Science Core Collection</collection><collection>Science Citation Index Expanded</collection><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Woods, Tyrone E</au><au>Heger, Alexander</au><au>Haemmerlé, Lionel</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>On monolithic supermassive stars</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>MON NOT R ASTRON SOC</stitle><date>2020-05-11</date><risdate>2020</risdate><volume>494</volume><issue>2</issue><spage>2236</spage><epage>2243</epage><pages>2236-2243</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
Supermassive stars have been proposed as the progenitors of the massive ($\sim \!10^{9}\, \mathrm{M}_{\odot }$) quasars observed at z ∼ 7. Prospects for directly detecting supermassive stars with next-generation facilities depend critically on their intrinsic lifetimes, as well as their formation rates. We use the one-dimensional stellar evolution code kepler to explore the theoretical limiting case of zero-metallicity non-rotating stars, formed monolithically with initial masses between $10$ and $190\, \mathrm{kM}_{\odot }$. We find that stars born with masses between $\sim\! 60$ and $\sim\! 150\, \mathrm{kM}_{\odot }$ collapse at the end of the main sequence, burning stably for $\sim\! 1.5\, \mathrm{Myr}$. More massive stars collapse directly through the general relativistic instability after only a thermal time-scale of $\sim\! 3$–$4\, \mathrm{kyr}$. The expected difficulty in producing such massive thermally relaxed objects, together with recent results for currently preferred rapidly accreting formation models, suggests that such ‘truly direct’ or ‘dark’ collapses may not be typical for supermassive objects in the early Universe. We close by discussing the evolution of supermassive stars in the broader context of massive primordial stellar evolution and the possibility of supermassive stellar explosions.</abstract><cop>OXFORD</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/staa763</doi><tpages>8</tpages><orcidid>https://orcid.org/0000-0002-3684-1325</orcidid><orcidid>https://orcid.org/0000-0003-1428-5775</orcidid></addata></record> |
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title | On monolithic supermassive stars |
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