The super‐Eddington nature of supermassive stars
ABSTRACT Supermassive stars (SMSs) are massive hydrogen objects that slowly radiate their gravitational binding energy. Such hypothetical primordial objects may have been the seed of the massive black holes (BHs) observed at the centre of galaxies. Under the standard picture, these objects can be ap...
Gespeichert in:
| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2012-12, Vol.427 (4), p.3071-3080 |
|---|---|
| Hauptverfasser: | , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | 3080 |
|---|---|
| container_issue | 4 |
| container_start_page | 3071 |
| container_title | Monthly notices of the Royal Astronomical Society |
| container_volume | 427 |
| creator | Dotan, Calanit Shaviv, Nir J. |
| description | ABSTRACT
Supermassive stars (SMSs) are massive hydrogen objects that slowly radiate their gravitational binding energy. Such hypothetical primordial objects may have been the seed of the massive black holes (BHs) observed at the centre of galaxies. Under the standard picture, these objects can be approximately described as n = 3 polytropes, and they are expected to shine extremely close to their Eddington luminosity. Once however one considers the porosity induced by instabilities near the Eddington limit, which give rise to super‐Eddington states, the standard picture should be modified. We study the structure, evolution and mass loss of these objects. We find the following. First, the evolution of SMSs is hastened due to their increased energy release. They accelerate continuum‐driven winds. If there is no rotational stabilization, these winds are insufficient to evaporate the objects such that they can collapse to form supermassive BHs, however, they do prevent SMSs from emitting a copious amount of ionizing radiation. If the SMSs are rotationally stabilized, the winds evaporate the objects until a normal sub‐Eddington star remains having a mass of a few
. |
| doi_str_mv | 10.1111/j.1365-2966.2012.22020.x |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_miscellaneous_1272714722</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1272714722</sourcerecordid><originalsourceid>FETCH-LOGICAL-c4910-75b32557e0471f4cccce0b01a564d2503a2bde507929dd4afe0661bd36f70d2c3</originalsourceid><addsrcrecordid>eNqNkM9Kw0AQhxdRsFbfIeDFS-LsbHa3uQhS6h-oClLPyybZaEKa1N1G25uP4DP6JG4a8eDJuczAfL9h-AgJKETU13kVUSZ4iIkQEQLFCBEQos0eGf0u9skIgPFwIik9JEfOVQAQMxQjgosXE7huZezXx-csz8vmed02QaPXnTVBWwy7pXaufPPgWlt3TA4KXTtz8tPH5OlqtpjehPOH69vp5TzM4oRCKHnKkHNpIJa0iDNfBlKgmos4Rw5MY5obDjLBJM9jXRgQgqY5E4WEHDM2JmfD3ZVtXzvj1mpZuszUtW5M2zlFUaKksUT06OkftGo72_jvPBWjYEAl99RkoDLbOmdNoVa2XGq7VRRUL1NVqnememeql6l2MtXGRy-G6HtZm-2_c-ru_nE3sm8wBXoE</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1242630175</pqid></control><display><type>article</type><title>The super‐Eddington nature of supermassive stars</title><source>Wiley Journals</source><source>Oxford Journals Open Access Collection</source><creator>Dotan, Calanit ; Shaviv, Nir J.</creator><creatorcontrib>Dotan, Calanit ; Shaviv, Nir J.</creatorcontrib><description>ABSTRACT
Supermassive stars (SMSs) are massive hydrogen objects that slowly radiate their gravitational binding energy. Such hypothetical primordial objects may have been the seed of the massive black holes (BHs) observed at the centre of galaxies. Under the standard picture, these objects can be approximately described as n = 3 polytropes, and they are expected to shine extremely close to their Eddington luminosity. Once however one considers the porosity induced by instabilities near the Eddington limit, which give rise to super‐Eddington states, the standard picture should be modified. We study the structure, evolution and mass loss of these objects. We find the following. First, the evolution of SMSs is hastened due to their increased energy release. They accelerate continuum‐driven winds. If there is no rotational stabilization, these winds are insufficient to evaporate the objects such that they can collapse to form supermassive BHs, however, they do prevent SMSs from emitting a copious amount of ionizing radiation. If the SMSs are rotationally stabilized, the winds evaporate the objects until a normal sub‐Eddington star remains having a mass of a few
.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1111/j.1365-2966.2012.22020.x</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Black holes ; dark ages, reionization, first stars ; Stars & galaxies ; stars: Population III ; stars: winds, outflows</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2012-12, Vol.427 (4), p.3071-3080</ispartof><rights>2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS</rights><rights>Monthly Notices of the Royal Astronomical Society © 2012 RAS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c4910-75b32557e0471f4cccce0b01a564d2503a2bde507929dd4afe0661bd36f70d2c3</citedby><cites>FETCH-LOGICAL-c4910-75b32557e0471f4cccce0b01a564d2503a2bde507929dd4afe0661bd36f70d2c3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1111%2Fj.1365-2966.2012.22020.x$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1111%2Fj.1365-2966.2012.22020.x$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,780,784,1417,27924,27925,45574,45575</link.rule.ids></links><search><creatorcontrib>Dotan, Calanit</creatorcontrib><creatorcontrib>Shaviv, Nir J.</creatorcontrib><title>The super‐Eddington nature of supermassive stars</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
Supermassive stars (SMSs) are massive hydrogen objects that slowly radiate their gravitational binding energy. Such hypothetical primordial objects may have been the seed of the massive black holes (BHs) observed at the centre of galaxies. Under the standard picture, these objects can be approximately described as n = 3 polytropes, and they are expected to shine extremely close to their Eddington luminosity. Once however one considers the porosity induced by instabilities near the Eddington limit, which give rise to super‐Eddington states, the standard picture should be modified. We study the structure, evolution and mass loss of these objects. We find the following. First, the evolution of SMSs is hastened due to their increased energy release. They accelerate continuum‐driven winds. If there is no rotational stabilization, these winds are insufficient to evaporate the objects such that they can collapse to form supermassive BHs, however, they do prevent SMSs from emitting a copious amount of ionizing radiation. If the SMSs are rotationally stabilized, the winds evaporate the objects until a normal sub‐Eddington star remains having a mass of a few
.</description><subject>Black holes</subject><subject>dark ages, reionization, first stars</subject><subject>Stars & galaxies</subject><subject>stars: Population III</subject><subject>stars: winds, outflows</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><recordid>eNqNkM9Kw0AQhxdRsFbfIeDFS-LsbHa3uQhS6h-oClLPyybZaEKa1N1G25uP4DP6JG4a8eDJuczAfL9h-AgJKETU13kVUSZ4iIkQEQLFCBEQos0eGf0u9skIgPFwIik9JEfOVQAQMxQjgosXE7huZezXx-csz8vmed02QaPXnTVBWwy7pXaufPPgWlt3TA4KXTtz8tPH5OlqtpjehPOH69vp5TzM4oRCKHnKkHNpIJa0iDNfBlKgmos4Rw5MY5obDjLBJM9jXRgQgqY5E4WEHDM2JmfD3ZVtXzvj1mpZuszUtW5M2zlFUaKksUT06OkftGo72_jvPBWjYEAl99RkoDLbOmdNoVa2XGq7VRRUL1NVqnememeql6l2MtXGRy-G6HtZm-2_c-ru_nE3sm8wBXoE</recordid><startdate>20121221</startdate><enddate>20121221</enddate><creator>Dotan, Calanit</creator><creator>Shaviv, Nir J.</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20121221</creationdate><title>The super‐Eddington nature of supermassive stars</title><author>Dotan, Calanit ; Shaviv, Nir J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c4910-75b32557e0471f4cccce0b01a564d2503a2bde507929dd4afe0661bd36f70d2c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2012</creationdate><topic>Black holes</topic><topic>dark ages, reionization, first stars</topic><topic>Stars & galaxies</topic><topic>stars: Population III</topic><topic>stars: winds, outflows</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Dotan, Calanit</creatorcontrib><creatorcontrib>Shaviv, Nir J.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Dotan, Calanit</au><au>Shaviv, Nir J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The super‐Eddington nature of supermassive stars</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2012-12-21</date><risdate>2012</risdate><volume>427</volume><issue>4</issue><spage>3071</spage><epage>3080</epage><pages>3071-3080</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
Supermassive stars (SMSs) are massive hydrogen objects that slowly radiate their gravitational binding energy. Such hypothetical primordial objects may have been the seed of the massive black holes (BHs) observed at the centre of galaxies. Under the standard picture, these objects can be approximately described as n = 3 polytropes, and they are expected to shine extremely close to their Eddington luminosity. Once however one considers the porosity induced by instabilities near the Eddington limit, which give rise to super‐Eddington states, the standard picture should be modified. We study the structure, evolution and mass loss of these objects. We find the following. First, the evolution of SMSs is hastened due to their increased energy release. They accelerate continuum‐driven winds. If there is no rotational stabilization, these winds are insufficient to evaporate the objects such that they can collapse to form supermassive BHs, however, they do prevent SMSs from emitting a copious amount of ionizing radiation. If the SMSs are rotationally stabilized, the winds evaporate the objects until a normal sub‐Eddington star remains having a mass of a few
.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1111/j.1365-2966.2012.22020.x</doi><tpages>10</tpages><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0035-8711 |
| ispartof | Monthly notices of the Royal Astronomical Society, 2012-12, Vol.427 (4), p.3071-3080 |
| issn | 0035-8711 1365-2966 |
| language | eng |
| recordid | cdi_proquest_miscellaneous_1272714722 |
| source | Wiley Journals; Oxford Journals Open Access Collection |
| subjects | Black holes dark ages, reionization, first stars Stars & galaxies stars: Population III stars: winds, outflows |
| title | The super‐Eddington nature of supermassive stars |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-04T13%3A14%3A12IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=The%20super%E2%80%90Eddington%20nature%20of%20supermassive%20stars&rft.jtitle=Monthly%20notices%20of%20the%20Royal%20Astronomical%20Society&rft.au=Dotan,%20Calanit&rft.date=2012-12-21&rft.volume=427&rft.issue=4&rft.spage=3071&rft.epage=3080&rft.pages=3071-3080&rft.issn=0035-8711&rft.eissn=1365-2966&rft_id=info:doi/10.1111/j.1365-2966.2012.22020.x&rft_dat=%3Cproquest_cross%3E1272714722%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=1242630175&rft_id=info:pmid/&rfr_iscdi=true |