The B-type Binaries Characterisation Programme – II. VFTS 291: a stripped star from a recent mass transfer phase
ABSTRACT Recent studies of massive binaries with putative black hole companions have uncovered a phase of binary evolution that has not been observed before, featuring a bloated stripped star that very recently ceased transferring mass to a main-sequence companion. In this study, we focus on the can...
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creator | Villaseñor, J I Lennon, D J Picco, A Shenar, T Marchant, P Langer, N Dufton, P L Nardini, F Evans, C J Bodensteiner, J de Mink, S E Götberg, Y Soszyński, I Taylor, W D Sana, H |
description | ABSTRACT
Recent studies of massive binaries with putative black hole companions have uncovered a phase of binary evolution that has not been observed before, featuring a bloated stripped star that very recently ceased transferring mass to a main-sequence companion. In this study, we focus on the candidate system VFTS 291, a binary with an orbital period of 108 d and a high semi-amplitude velocity (K1 = 93.7 ± 0.2 km s−1). Through our analysis of the disentangled spectra of the two components, together with dynamical and evolutionary arguments, we identify a narrow-lined star of ∼1.5–2.5 $\, \mathrm{M}_\odot$ dominating the spectrum, and an early B-type main-sequence companion of 13.2 ± 1.5 $\, \mathrm{M}_\odot$. The low mass of the narrow-lined star, and the high mass ratio, suggest that VFTS 291 is a post-mass-transfer system, with the narrow-lined star being bloated and stripped of its hydrogen-rich envelope, sharing many similarities with other recently discovered stripped stars. Our finding is supported by our detailed binary evolution models, which indicate that the system can be well explained by an initial configuration consisting of an 8.1 $\, \mathrm{M}_\odot$ primary with an 8 $\, \mathrm{M}_\odot$ companion in a 7 d orbital period. While some open questions remain, particularly concerning the surface helium enrichment of the stripped star and the rotational velocity of the companion, we expect that high-resolution spectroscopy may help reconcile our estimates with theory. Our study highlights the importance of multi-epoch spectroscopic surveys to identify and characterize binary interaction products, and provides important insights into the evolution of massive binary stars. |
doi_str_mv | 10.1093/mnras/stad2533 |
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Recent studies of massive binaries with putative black hole companions have uncovered a phase of binary evolution that has not been observed before, featuring a bloated stripped star that very recently ceased transferring mass to a main-sequence companion. In this study, we focus on the candidate system VFTS 291, a binary with an orbital period of 108 d and a high semi-amplitude velocity (K1 = 93.7 ± 0.2 km s−1). Through our analysis of the disentangled spectra of the two components, together with dynamical and evolutionary arguments, we identify a narrow-lined star of ∼1.5–2.5 $\, \mathrm{M}_\odot$ dominating the spectrum, and an early B-type main-sequence companion of 13.2 ± 1.5 $\, \mathrm{M}_\odot$. The low mass of the narrow-lined star, and the high mass ratio, suggest that VFTS 291 is a post-mass-transfer system, with the narrow-lined star being bloated and stripped of its hydrogen-rich envelope, sharing many similarities with other recently discovered stripped stars. Our finding is supported by our detailed binary evolution models, which indicate that the system can be well explained by an initial configuration consisting of an 8.1 $\, \mathrm{M}_\odot$ primary with an 8 $\, \mathrm{M}_\odot$ companion in a 7 d orbital period. While some open questions remain, particularly concerning the surface helium enrichment of the stripped star and the rotational velocity of the companion, we expect that high-resolution spectroscopy may help reconcile our estimates with theory. Our study highlights the importance of multi-epoch spectroscopic surveys to identify and characterize binary interaction products, and provides important insights into the evolution of massive binary stars.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stad2533</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Binary stars ; Companion stars ; Mass transfer ; Orbits ; Rotation ; Rotational spectra ; Spectrum analysis ; Stellar envelopes ; Stellar evolution</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2023-11, Vol.525 (4), p.5121-5145</ispartof><rights>2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society 2023</rights><rights>2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c301t-518783c6dc7e6b12857d00ad3ee1a921402e69be2d311088d6fef31bb13c32193</citedby><cites>FETCH-LOGICAL-c301t-518783c6dc7e6b12857d00ad3ee1a921402e69be2d311088d6fef31bb13c32193</cites><orcidid>0009-0005-7288-6407 ; 0000-0001-6656-4130 ; 0000-0002-0338-8181 ; 0000-0001-9336-2825 ; 0000-0002-7984-1675 ; 0000-0003-0642-8107</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stad2533$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Villaseñor, J I</creatorcontrib><creatorcontrib>Lennon, D J</creatorcontrib><creatorcontrib>Picco, A</creatorcontrib><creatorcontrib>Shenar, T</creatorcontrib><creatorcontrib>Marchant, P</creatorcontrib><creatorcontrib>Langer, N</creatorcontrib><creatorcontrib>Dufton, P L</creatorcontrib><creatorcontrib>Nardini, F</creatorcontrib><creatorcontrib>Evans, C J</creatorcontrib><creatorcontrib>Bodensteiner, J</creatorcontrib><creatorcontrib>de Mink, S E</creatorcontrib><creatorcontrib>Götberg, Y</creatorcontrib><creatorcontrib>Soszyński, I</creatorcontrib><creatorcontrib>Taylor, W D</creatorcontrib><creatorcontrib>Sana, H</creatorcontrib><title>The B-type Binaries Characterisation Programme – II. VFTS 291: a stripped star from a recent mass transfer phase</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
Recent studies of massive binaries with putative black hole companions have uncovered a phase of binary evolution that has not been observed before, featuring a bloated stripped star that very recently ceased transferring mass to a main-sequence companion. In this study, we focus on the candidate system VFTS 291, a binary with an orbital period of 108 d and a high semi-amplitude velocity (K1 = 93.7 ± 0.2 km s−1). Through our analysis of the disentangled spectra of the two components, together with dynamical and evolutionary arguments, we identify a narrow-lined star of ∼1.5–2.5 $\, \mathrm{M}_\odot$ dominating the spectrum, and an early B-type main-sequence companion of 13.2 ± 1.5 $\, \mathrm{M}_\odot$. The low mass of the narrow-lined star, and the high mass ratio, suggest that VFTS 291 is a post-mass-transfer system, with the narrow-lined star being bloated and stripped of its hydrogen-rich envelope, sharing many similarities with other recently discovered stripped stars. Our finding is supported by our detailed binary evolution models, which indicate that the system can be well explained by an initial configuration consisting of an 8.1 $\, \mathrm{M}_\odot$ primary with an 8 $\, \mathrm{M}_\odot$ companion in a 7 d orbital period. While some open questions remain, particularly concerning the surface helium enrichment of the stripped star and the rotational velocity of the companion, we expect that high-resolution spectroscopy may help reconcile our estimates with theory. Our study highlights the importance of multi-epoch spectroscopic surveys to identify and characterize binary interaction products, and provides important insights into the evolution of massive binary stars.</description><subject>Binary stars</subject><subject>Companion stars</subject><subject>Mass transfer</subject><subject>Orbits</subject><subject>Rotation</subject><subject>Rotational spectra</subject><subject>Spectrum analysis</subject><subject>Stellar envelopes</subject><subject>Stellar evolution</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><recordid>eNqFkD1Pw0AMhk8IJEphZT6JiSHt-dykCRtUFCohgURhjZzEoanIB77r0I3_wD_klxAozEyvZT2vLT1KnYIZgUlwXDdCbuw8FTZE3FMDwCgMbBJF-2pgDIZBPAU4VEfOrY0xE7TRQMlyxfoq8Nuuj6ohqdjp2YqEcs9SOfJV2-gHaV-E6pr15_uHXixG-nm-fNQ2gQtN2nmpuo6LfiDRpbR1vxTOufG6Jue0F2pcyaK7FTk-VgclvTo--c2heppfL2e3wd39zWJ2eRfkaMAHIcTTGPOoyKccZWDjcFoYQwUyAyUWJsZylGRsCwQwcVxEJZcIWQaYo4UEh-psd7eT9m3DzqfrdiNN_zJFQAwnNjFhT412VC6tc8Jl2klVk2xTMOm31_THa_rntS-c7wrtpvuP_QKyKHsk</recordid><startdate>20231101</startdate><enddate>20231101</enddate><creator>Villaseñor, J I</creator><creator>Lennon, D J</creator><creator>Picco, A</creator><creator>Shenar, T</creator><creator>Marchant, P</creator><creator>Langer, N</creator><creator>Dufton, P L</creator><creator>Nardini, F</creator><creator>Evans, C J</creator><creator>Bodensteiner, J</creator><creator>de Mink, S E</creator><creator>Götberg, Y</creator><creator>Soszyński, I</creator><creator>Taylor, W D</creator><creator>Sana, H</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><orcidid>https://orcid.org/0009-0005-7288-6407</orcidid><orcidid>https://orcid.org/0000-0001-6656-4130</orcidid><orcidid>https://orcid.org/0000-0002-0338-8181</orcidid><orcidid>https://orcid.org/0000-0001-9336-2825</orcidid><orcidid>https://orcid.org/0000-0002-7984-1675</orcidid><orcidid>https://orcid.org/0000-0003-0642-8107</orcidid></search><sort><creationdate>20231101</creationdate><title>The B-type Binaries Characterisation Programme – II. VFTS 291: a stripped star from a recent mass transfer phase</title><author>Villaseñor, J I ; Lennon, D J ; Picco, A ; Shenar, T ; Marchant, P ; Langer, N ; Dufton, P L ; Nardini, F ; Evans, C J ; Bodensteiner, J ; de Mink, S E ; Götberg, Y ; Soszyński, I ; Taylor, W D ; Sana, H</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c301t-518783c6dc7e6b12857d00ad3ee1a921402e69be2d311088d6fef31bb13c32193</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Binary stars</topic><topic>Companion stars</topic><topic>Mass transfer</topic><topic>Orbits</topic><topic>Rotation</topic><topic>Rotational spectra</topic><topic>Spectrum analysis</topic><topic>Stellar envelopes</topic><topic>Stellar evolution</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Villaseñor, J I</creatorcontrib><creatorcontrib>Lennon, D J</creatorcontrib><creatorcontrib>Picco, A</creatorcontrib><creatorcontrib>Shenar, T</creatorcontrib><creatorcontrib>Marchant, P</creatorcontrib><creatorcontrib>Langer, N</creatorcontrib><creatorcontrib>Dufton, P L</creatorcontrib><creatorcontrib>Nardini, F</creatorcontrib><creatorcontrib>Evans, C J</creatorcontrib><creatorcontrib>Bodensteiner, J</creatorcontrib><creatorcontrib>de Mink, S E</creatorcontrib><creatorcontrib>Götberg, Y</creatorcontrib><creatorcontrib>Soszyński, I</creatorcontrib><creatorcontrib>Taylor, W D</creatorcontrib><creatorcontrib>Sana, H</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Villaseñor, J I</au><au>Lennon, D J</au><au>Picco, A</au><au>Shenar, T</au><au>Marchant, P</au><au>Langer, N</au><au>Dufton, P L</au><au>Nardini, F</au><au>Evans, C J</au><au>Bodensteiner, J</au><au>de Mink, S E</au><au>Götberg, Y</au><au>Soszyński, I</au><au>Taylor, W D</au><au>Sana, H</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The B-type Binaries Characterisation Programme – II. VFTS 291: a stripped star from a recent mass transfer phase</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2023-11-01</date><risdate>2023</risdate><volume>525</volume><issue>4</issue><spage>5121</spage><epage>5145</epage><pages>5121-5145</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
Recent studies of massive binaries with putative black hole companions have uncovered a phase of binary evolution that has not been observed before, featuring a bloated stripped star that very recently ceased transferring mass to a main-sequence companion. In this study, we focus on the candidate system VFTS 291, a binary with an orbital period of 108 d and a high semi-amplitude velocity (K1 = 93.7 ± 0.2 km s−1). Through our analysis of the disentangled spectra of the two components, together with dynamical and evolutionary arguments, we identify a narrow-lined star of ∼1.5–2.5 $\, \mathrm{M}_\odot$ dominating the spectrum, and an early B-type main-sequence companion of 13.2 ± 1.5 $\, \mathrm{M}_\odot$. The low mass of the narrow-lined star, and the high mass ratio, suggest that VFTS 291 is a post-mass-transfer system, with the narrow-lined star being bloated and stripped of its hydrogen-rich envelope, sharing many similarities with other recently discovered stripped stars. Our finding is supported by our detailed binary evolution models, which indicate that the system can be well explained by an initial configuration consisting of an 8.1 $\, \mathrm{M}_\odot$ primary with an 8 $\, \mathrm{M}_\odot$ companion in a 7 d orbital period. While some open questions remain, particularly concerning the surface helium enrichment of the stripped star and the rotational velocity of the companion, we expect that high-resolution spectroscopy may help reconcile our estimates with theory. Our study highlights the importance of multi-epoch spectroscopic surveys to identify and characterize binary interaction products, and provides important insights into the evolution of massive binary stars.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stad2533</doi><tpages>25</tpages><orcidid>https://orcid.org/0009-0005-7288-6407</orcidid><orcidid>https://orcid.org/0000-0001-6656-4130</orcidid><orcidid>https://orcid.org/0000-0002-0338-8181</orcidid><orcidid>https://orcid.org/0000-0001-9336-2825</orcidid><orcidid>https://orcid.org/0000-0002-7984-1675</orcidid><orcidid>https://orcid.org/0000-0003-0642-8107</orcidid><oa>free_for_read</oa></addata></record> |
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subjects | Binary stars Companion stars Mass transfer Orbits Rotation Rotational spectra Spectrum analysis Stellar envelopes Stellar evolution |
title | The B-type Binaries Characterisation Programme – II. VFTS 291: a stripped star from a recent mass transfer phase |
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