Evidence from high-mass X-ray binaries that Galactic WR components of WR+O binaries end their life with a supernova explosion
Context. Theoretical population number studies of binaries with at least one black hole (BH) component obviously depend on whether or not BHs receive a (natal) kick during their formation. Aims. Several observational facts seem to indicate that BHs do indeed receive a kick during their formation. In...
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Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2020-04, Vol.636, p.A99 |
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container_start_page | A99 |
container_title | Astronomy and astrophysics (Berlin) |
container_volume | 636 |
creator | Vanbeveren, D. Mennekens, N. van den Heuvel, E. P. J. Van Bever, J. |
description | Context.
Theoretical population number studies of binaries with at least one black hole (BH) component obviously depend on whether or not BHs receive a (natal) kick during their formation.
Aims.
Several observational facts seem to indicate that BHs do indeed receive a kick during their formation. In the present paper, we discuss additional evidence of this.
Methods.
The progenitors of wind-fed high-mass X-ray binaries (HMXB) with a BH component (BH HMXB) are WR+OB binaries where the Wolf–Rayet (WR) star will finally collapse and form the BH. Starting from the observed population of WR+OB binaries in the solar neighborhood, we predict the population of wind-fed BH HMXBs as a function of the BH-natal kick.
Results.
The simulations reveal that when WR stars collapse into a BH with a zero or low kick, we should expect 100 or more wind-fed BH HMXBs in the solar neighborhood, whereas only one is observed (Cyg X-1). We consider this as evidence that either WR components in binaries end their life as a neutron star or that they collapse into BHs, both accompanied by a supernova explosion imparting significant (natal) kicks. |
doi_str_mv | 10.1051/0004-6361/201937253 |
format | Article |
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Theoretical population number studies of binaries with at least one black hole (BH) component obviously depend on whether or not BHs receive a (natal) kick during their formation.
Aims.
Several observational facts seem to indicate that BHs do indeed receive a kick during their formation. In the present paper, we discuss additional evidence of this.
Methods.
The progenitors of wind-fed high-mass X-ray binaries (HMXB) with a BH component (BH HMXB) are WR+OB binaries where the Wolf–Rayet (WR) star will finally collapse and form the BH. Starting from the observed population of WR+OB binaries in the solar neighborhood, we predict the population of wind-fed BH HMXBs as a function of the BH-natal kick.
Results.
The simulations reveal that when WR stars collapse into a BH with a zero or low kick, we should expect 100 or more wind-fed BH HMXBs in the solar neighborhood, whereas only one is observed (Cyg X-1). We consider this as evidence that either WR components in binaries end their life as a neutron star or that they collapse into BHs, both accompanied by a supernova explosion imparting significant (natal) kicks.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201937253</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Black holes ; Neutron stars ; Progenitors (astrophysics) ; Solar neighborhood ; Stellar evolution ; X ray binaries ; X ray stars</subject><ispartof>Astronomy and astrophysics (Berlin), 2020-04, Vol.636, p.A99</ispartof><rights>Copyright EDP Sciences Apr 2020</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c2373-21aa9d1942aaa1ac84d37bf9a04012ef127090660ff31f70f0fbda597ab4985a3</citedby><cites>FETCH-LOGICAL-c2373-21aa9d1942aaa1ac84d37bf9a04012ef127090660ff31f70f0fbda597ab4985a3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,777,781,3714,27905,27906</link.rule.ids></links><search><creatorcontrib>Vanbeveren, D.</creatorcontrib><creatorcontrib>Mennekens, N.</creatorcontrib><creatorcontrib>van den Heuvel, E. P. J.</creatorcontrib><creatorcontrib>Van Bever, J.</creatorcontrib><title>Evidence from high-mass X-ray binaries that Galactic WR components of WR+O binaries end their life with a supernova explosion</title><title>Astronomy and astrophysics (Berlin)</title><description>Context.
Theoretical population number studies of binaries with at least one black hole (BH) component obviously depend on whether or not BHs receive a (natal) kick during their formation.
Aims.
Several observational facts seem to indicate that BHs do indeed receive a kick during their formation. In the present paper, we discuss additional evidence of this.
Methods.
The progenitors of wind-fed high-mass X-ray binaries (HMXB) with a BH component (BH HMXB) are WR+OB binaries where the Wolf–Rayet (WR) star will finally collapse and form the BH. Starting from the observed population of WR+OB binaries in the solar neighborhood, we predict the population of wind-fed BH HMXBs as a function of the BH-natal kick.
Results.
The simulations reveal that when WR stars collapse into a BH with a zero or low kick, we should expect 100 or more wind-fed BH HMXBs in the solar neighborhood, whereas only one is observed (Cyg X-1). We consider this as evidence that either WR components in binaries end their life as a neutron star or that they collapse into BHs, both accompanied by a supernova explosion imparting significant (natal) kicks.</description><subject>Black holes</subject><subject>Neutron stars</subject><subject>Progenitors (astrophysics)</subject><subject>Solar neighborhood</subject><subject>Stellar evolution</subject><subject>X ray binaries</subject><subject>X ray stars</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNpFkF1LwzAUhoMoOKe_wJuAl1KXrzbtpYw5hcFAFL0Lp21iM7qkJt10F_53Oybz6nAOz3lfeBC6puSOkpROCCEiyXhGJ4zQgkuW8hM0ooKzhEiRnaLRkThHFzGuhpXRnI_Qz2xra-0qjU3wa9zYjyZZQ4z4PQmww6V1EKyOuG-gx3Nooepthd-eceXXnXfa9RF7Mxxul_-wdvXwoG3ArTUaf9m-wYDjptPB-S1g_d21PlrvLtGZgTbqq785Rq8Ps5fpY7JYzp-m94ukYlzyhFGAoqaFYABAocpFzWVpCiCCUKYNZZIUJMuIMZwaSQwxZQ1pIaEURZ4CH6ObQ24X_OdGx16t_Ca4oVIxkUtKM0nYQPEDVQUfY9BGdcGuIewUJWrvWe0tqr1FdfTMfwF9KnA5</recordid><startdate>202004</startdate><enddate>202004</enddate><creator>Vanbeveren, D.</creator><creator>Mennekens, N.</creator><creator>van den Heuvel, E. P. J.</creator><creator>Van Bever, J.</creator><general>EDP Sciences</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>202004</creationdate><title>Evidence from high-mass X-ray binaries that Galactic WR components of WR+O binaries end their life with a supernova explosion</title><author>Vanbeveren, D. ; Mennekens, N. ; van den Heuvel, E. P. J. ; Van Bever, J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c2373-21aa9d1942aaa1ac84d37bf9a04012ef127090660ff31f70f0fbda597ab4985a3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Black holes</topic><topic>Neutron stars</topic><topic>Progenitors (astrophysics)</topic><topic>Solar neighborhood</topic><topic>Stellar evolution</topic><topic>X ray binaries</topic><topic>X ray stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Vanbeveren, D.</creatorcontrib><creatorcontrib>Mennekens, N.</creatorcontrib><creatorcontrib>van den Heuvel, E. P. J.</creatorcontrib><creatorcontrib>Van Bever, J.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Vanbeveren, D.</au><au>Mennekens, N.</au><au>van den Heuvel, E. P. J.</au><au>Van Bever, J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Evidence from high-mass X-ray binaries that Galactic WR components of WR+O binaries end their life with a supernova explosion</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2020-04</date><risdate>2020</risdate><volume>636</volume><spage>A99</spage><pages>A99-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>Context.
Theoretical population number studies of binaries with at least one black hole (BH) component obviously depend on whether or not BHs receive a (natal) kick during their formation.
Aims.
Several observational facts seem to indicate that BHs do indeed receive a kick during their formation. In the present paper, we discuss additional evidence of this.
Methods.
The progenitors of wind-fed high-mass X-ray binaries (HMXB) with a BH component (BH HMXB) are WR+OB binaries where the Wolf–Rayet (WR) star will finally collapse and form the BH. Starting from the observed population of WR+OB binaries in the solar neighborhood, we predict the population of wind-fed BH HMXBs as a function of the BH-natal kick.
Results.
The simulations reveal that when WR stars collapse into a BH with a zero or low kick, we should expect 100 or more wind-fed BH HMXBs in the solar neighborhood, whereas only one is observed (Cyg X-1). We consider this as evidence that either WR components in binaries end their life as a neutron star or that they collapse into BHs, both accompanied by a supernova explosion imparting significant (natal) kicks.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201937253</doi><oa>free_for_read</oa></addata></record> |
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language | eng |
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source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; EDP Sciences |
subjects | Black holes Neutron stars Progenitors (astrophysics) Solar neighborhood Stellar evolution X ray binaries X ray stars |
title | Evidence from high-mass X-ray binaries that Galactic WR components of WR+O binaries end their life with a supernova explosion |
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