Prevalence of SED Turndown among Classical Be Stars: Are All Be Stars Close Binaries?
Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property allowing for the formation of their circumstellar disks. Past evolution in a mass and angular momentum transferring binary system offers a plausible solution to how Be stars attained their fast rotation. Alth...
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creator | Klement, Robert Carciofi, A. C. Rivinius, T. Ignace, R. Matthews, L. D. Torstensson, K. Gies, D. Vieira, R. G. Richardson, N. D. de Souza, A. Domiciano Bjorkman, J. E. Hallinan, G. Faes, D. M. Mota, B. Gullingsrud, A. D. de Breuck, C. Kervella, P. Curé, M. Gunawan, D. |
description | Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property allowing for the formation of their circumstellar disks. Past evolution in a mass and angular momentum transferring binary system offers a plausible solution to how Be stars attained their fast rotation. Although the subdwarf remnants of mass donors in such systems should exist in abundance, only a few have been confirmed due to tight observational constraints. An indirect method of detecting otherwise hidden companions is offered by their effect on the outer parts of Be star disks, which are expected to be disrupted or truncated. In the context of the infrared and radio continuum excess radiation originating in the disk, the disk truncation can be revealed by a turndown in the spectral energy distribution due to reduced radio flux levels. In this work, we search for signs of spectral turndown in a sample of 57 classical Be stars with radio data, which include new data for 23 stars and the longest-wavelength detections so far (λ 10 cm) for two stars. We confidently detect the turndown for all 26 stars with sufficient data coverage (20 of which are not known to have close binary companions). For the remaining 31 stars, the data are inconclusive as to whether the turndown is present or not. The analysis suggests that many if not all Be stars have close companions influencing their outer disks. If confirmed to be subdwarf companions, the mass transfer spin-up scenario might explain the existence of the vast majority of classical Be stars. |
doi_str_mv | 10.3847/1538-4357/ab48e7 |
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C. ; Rivinius, T. ; Ignace, R. ; Matthews, L. D. ; Torstensson, K. ; Gies, D. ; Vieira, R. G. ; Richardson, N. D. ; de Souza, A. Domiciano ; Bjorkman, J. E. ; Hallinan, G. ; Faes, D. M. ; Mota, B. ; Gullingsrud, A. D. ; de Breuck, C. ; Kervella, P. ; Curé, M. ; Gunawan, D.</creator><creatorcontrib>Klement, Robert ; Carciofi, A. C. ; Rivinius, T. ; Ignace, R. ; Matthews, L. D. ; Torstensson, K. ; Gies, D. ; Vieira, R. G. ; Richardson, N. D. ; de Souza, A. Domiciano ; Bjorkman, J. E. ; Hallinan, G. ; Faes, D. M. ; Mota, B. ; Gullingsrud, A. D. ; de Breuck, C. ; Kervella, P. ; Curé, M. ; Gunawan, D.</creatorcontrib><description>Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property allowing for the formation of their circumstellar disks. Past evolution in a mass and angular momentum transferring binary system offers a plausible solution to how Be stars attained their fast rotation. Although the subdwarf remnants of mass donors in such systems should exist in abundance, only a few have been confirmed due to tight observational constraints. An indirect method of detecting otherwise hidden companions is offered by their effect on the outer parts of Be star disks, which are expected to be disrupted or truncated. In the context of the infrared and radio continuum excess radiation originating in the disk, the disk truncation can be revealed by a turndown in the spectral energy distribution due to reduced radio flux levels. In this work, we search for signs of spectral turndown in a sample of 57 classical Be stars with radio data, which include new data for 23 stars and the longest-wavelength detections so far (λ 10 cm) for two stars. We confidently detect the turndown for all 26 stars with sufficient data coverage (20 of which are not known to have close binary companions). For the remaining 31 stars, the data are inconclusive as to whether the turndown is present or not. The analysis suggests that many if not all Be stars have close companions influencing their outer disks. If confirmed to be subdwarf companions, the mass transfer spin-up scenario might explain the existence of the vast majority of classical Be stars.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ab48e7</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Accretion disks ; Angular momentum ; Astrophysics ; Be stars ; Binary stars ; Circumstellar disks ; Circumstellar matter ; Early-type emission stars ; Infrared excess ; Mass transfer ; Physics ; Radiation ; Radio ; Radio astronomy ; Radio continuum emission ; Spectral energy distribution ; Stellar astronomy ; Stellar evolution ; Stellar rotation ; Stellar system evolution ; Subdwarf stars</subject><ispartof>The Astrophysical journal, 2019-11, Vol.885 (2), p.147</ispartof><rights>2019. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Nov 10, 2019</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c384t-8a2ff75b4472d9e2dedb6f37998350cd716dc77cd8c38a7cea8f6cdf05f8d3a93</citedby><cites>FETCH-LOGICAL-c384t-8a2ff75b4472d9e2dedb6f37998350cd716dc77cd8c38a7cea8f6cdf05f8d3a93</cites><orcidid>0000-0002-7204-5502 ; 0000-0001-8537-3583 ; 0000-0002-4313-0169 ; 0000-0003-0626-1749 ; 0000-0002-9369-574X ; 0000-0002-6637-3315 ; 0000-0002-2806-9339 ; 0000-0002-2191-8692</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ab48e7/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ab48e7$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://hal.science/hal-03127402$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Klement, Robert</creatorcontrib><creatorcontrib>Carciofi, A. C.</creatorcontrib><creatorcontrib>Rivinius, T.</creatorcontrib><creatorcontrib>Ignace, R.</creatorcontrib><creatorcontrib>Matthews, L. D.</creatorcontrib><creatorcontrib>Torstensson, K.</creatorcontrib><creatorcontrib>Gies, D.</creatorcontrib><creatorcontrib>Vieira, R. G.</creatorcontrib><creatorcontrib>Richardson, N. D.</creatorcontrib><creatorcontrib>de Souza, A. Domiciano</creatorcontrib><creatorcontrib>Bjorkman, J. E.</creatorcontrib><creatorcontrib>Hallinan, G.</creatorcontrib><creatorcontrib>Faes, D. M.</creatorcontrib><creatorcontrib>Mota, B.</creatorcontrib><creatorcontrib>Gullingsrud, A. D.</creatorcontrib><creatorcontrib>de Breuck, C.</creatorcontrib><creatorcontrib>Kervella, P.</creatorcontrib><creatorcontrib>Curé, M.</creatorcontrib><creatorcontrib>Gunawan, D.</creatorcontrib><title>Prevalence of SED Turndown among Classical Be Stars: Are All Be Stars Close Binaries?</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property allowing for the formation of their circumstellar disks. Past evolution in a mass and angular momentum transferring binary system offers a plausible solution to how Be stars attained their fast rotation. Although the subdwarf remnants of mass donors in such systems should exist in abundance, only a few have been confirmed due to tight observational constraints. An indirect method of detecting otherwise hidden companions is offered by their effect on the outer parts of Be star disks, which are expected to be disrupted or truncated. In the context of the infrared and radio continuum excess radiation originating in the disk, the disk truncation can be revealed by a turndown in the spectral energy distribution due to reduced radio flux levels. In this work, we search for signs of spectral turndown in a sample of 57 classical Be stars with radio data, which include new data for 23 stars and the longest-wavelength detections so far (λ 10 cm) for two stars. We confidently detect the turndown for all 26 stars with sufficient data coverage (20 of which are not known to have close binary companions). For the remaining 31 stars, the data are inconclusive as to whether the turndown is present or not. The analysis suggests that many if not all Be stars have close companions influencing their outer disks. 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D.</creator><creator>de Breuck, C.</creator><creator>Kervella, P.</creator><creator>Curé, M.</creator><creator>Gunawan, D.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><general>American Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><orcidid>https://orcid.org/0000-0002-7204-5502</orcidid><orcidid>https://orcid.org/0000-0001-8537-3583</orcidid><orcidid>https://orcid.org/0000-0002-4313-0169</orcidid><orcidid>https://orcid.org/0000-0003-0626-1749</orcidid><orcidid>https://orcid.org/0000-0002-9369-574X</orcidid><orcidid>https://orcid.org/0000-0002-6637-3315</orcidid><orcidid>https://orcid.org/0000-0002-2806-9339</orcidid><orcidid>https://orcid.org/0000-0002-2191-8692</orcidid></search><sort><creationdate>20191110</creationdate><title>Prevalence of SED Turndown among Classical Be Stars: Are All Be Stars Close Binaries?</title><author>Klement, Robert ; Carciofi, A. C. ; Rivinius, T. ; Ignace, R. ; Matthews, L. D. ; Torstensson, K. ; Gies, D. ; Vieira, R. G. ; Richardson, N. D. ; de Souza, A. Domiciano ; Bjorkman, J. E. ; Hallinan, G. ; Faes, D. M. ; Mota, B. ; Gullingsrud, A. 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Domiciano</au><au>Bjorkman, J. E.</au><au>Hallinan, G.</au><au>Faes, D. M.</au><au>Mota, B.</au><au>Gullingsrud, A. D.</au><au>de Breuck, C.</au><au>Kervella, P.</au><au>Curé, M.</au><au>Gunawan, D.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Prevalence of SED Turndown among Classical Be Stars: Are All Be Stars Close Binaries?</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2019-11-10</date><risdate>2019</risdate><volume>885</volume><issue>2</issue><spage>147</spage><pages>147-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property allowing for the formation of their circumstellar disks. Past evolution in a mass and angular momentum transferring binary system offers a plausible solution to how Be stars attained their fast rotation. Although the subdwarf remnants of mass donors in such systems should exist in abundance, only a few have been confirmed due to tight observational constraints. An indirect method of detecting otherwise hidden companions is offered by their effect on the outer parts of Be star disks, which are expected to be disrupted or truncated. In the context of the infrared and radio continuum excess radiation originating in the disk, the disk truncation can be revealed by a turndown in the spectral energy distribution due to reduced radio flux levels. In this work, we search for signs of spectral turndown in a sample of 57 classical Be stars with radio data, which include new data for 23 stars and the longest-wavelength detections so far (λ 10 cm) for two stars. We confidently detect the turndown for all 26 stars with sufficient data coverage (20 of which are not known to have close binary companions). 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subjects | Accretion disks Angular momentum Astrophysics Be stars Binary stars Circumstellar disks Circumstellar matter Early-type emission stars Infrared excess Mass transfer Physics Radiation Radio Radio astronomy Radio continuum emission Spectral energy distribution Stellar astronomy Stellar evolution Stellar rotation Stellar system evolution Subdwarf stars |
title | Prevalence of SED Turndown among Classical Be Stars: Are All Be Stars Close Binaries? |
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