V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System

Autores
Li, F. X.; Liao, W. P.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio; Zhang, J.; Zhao, E. G.
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
V606 Centauri (V606 Cen) is an early B-type close binary with an orbital period of 1.4950935 days, and its complete light curves are very difficult to observe on the ground. By analyzing the continuous light curve obtained by TESS, we found that it is a marginal contact binary with a very low fill-out factor of about 2%. The O - C diagram of V606 Cen is constructed for the first time based on 118.8 yr of eclipse times. The O - C diagram has been found to show a downward parabolic change together with a cyclic oscillation with a semiamplitude of 0.0545 days and a period of 88.3 yr. The downward parabolic variation reveals a linear period decrease at a rate of dP/dt = -2.08 × 10-7 days yr-1 that can be explained by the mass transfer from the more massive component to the less massive one. Both the marginal contact configuration and the continuous period decrease suggest that V606 Cen is a newly formed contact binary via Case A mass transfer. The cyclic change in the O - C diagram can be explained by the light-travel time effect via the presence of a third body. The lowest mass of the tertiary companion is determined to be M 3 = 4.51 (±0.43) M o˙ and the tertiary is orbiting around the central eclipsing binary in a nearly circular orbit (e = 0.33). All of the results indicate that V606 Cen is a newly formed massive contact binary in a hierarchical triple system.
Fil: Li, F. X.. Chinese Academy of Sciences; República de China. Yunnan Observatories; China. Chinese Academy of Sciences; República de China
Fil: Liao, W. P.. Yunnan Observatories; China. Chinese Academy of Sciences; República de China
Fil: Qian, S. B.. Yunnan Observatories; China. Chinese Academy of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Zhang, J.. Chinese Academy of Sciences; República de China. Yunnan Observatories; China
Fil: Zhao, E. G.. Chinese Academy of Sciences; República de China. Yunnan Observatories; China
Materia
Multiple stars
Contact binary stars
Eclipsing binary stars
Early stellar evolution
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/211929
Acceder
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network_name_str CONICET Digital (CONICET)
spelling V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple SystemLi, F. X.Liao, W. P.Qian, S. B.Fernandez Lajus, Eduardo EusebioZhang, J.Zhao, E. G.Multiple starsContact binary starsEclipsing binary starsEarly stellar evolutionhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1V606 Centauri (V606 Cen) is an early B-type close binary with an orbital period of 1.4950935 days, and its complete light curves are very difficult to observe on the ground. By analyzing the continuous light curve obtained by TESS, we found that it is a marginal contact binary with a very low fill-out factor of about 2%. The O - C diagram of V606 Cen is constructed for the first time based on 118.8 yr of eclipse times. The O - C diagram has been found to show a downward parabolic change together with a cyclic oscillation with a semiamplitude of 0.0545 days and a period of 88.3 yr. The downward parabolic variation reveals a linear period decrease at a rate of dP/dt = -2.08 × 10-7 days yr-1 that can be explained by the mass transfer from the more massive component to the less massive one. Both the marginal contact configuration and the continuous period decrease suggest that V606 Cen is a newly formed contact binary via Case A mass transfer. The cyclic change in the O - C diagram can be explained by the light-travel time effect via the presence of a third body. The lowest mass of the tertiary companion is determined to be M 3 = 4.51 (±0.43) M o˙ and the tertiary is orbiting around the central eclipsing binary in a nearly circular orbit (e = 0.33). All of the results indicate that V606 Cen is a newly formed massive contact binary in a hierarchical triple system.Fil: Li, F. X.. Chinese Academy of Sciences; República de China. Yunnan Observatories; China. Chinese Academy of Sciences; República de ChinaFil: Liao, W. P.. Yunnan Observatories; China. Chinese Academy of Sciences; República de ChinaFil: Qian, S. B.. Yunnan Observatories; China. Chinese Academy of Sciences; República de ChinaFil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Zhang, J.. Chinese Academy of Sciences; República de China. Yunnan Observatories; ChinaFil: Zhao, E. G.. Chinese Academy of Sciences; República de China. Yunnan Observatories; ChinaIOP Publishing2022-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/211929Li, F. X.; Liao, W. P.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio; Zhang, J.; et al.; V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System; IOP Publishing; Astrophysical Journal; 924; 1; 1-2022; 1-110004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ac3425info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ac3425info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:59:06Zoai:ri.conicet.gov.ar:11336/211929instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 14:59:07.233CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
title V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
spellingShingle V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
Li, F. X.
Multiple stars
Contact binary stars
Eclipsing binary stars
Early stellar evolution
title_short V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
title_full V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
title_fullStr V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
title_full_unstemmed V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
title_sort V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System
dc.creator.none.fl_str_mv Li, F. X.
Liao, W. P.
Qian, S. B.
Fernandez Lajus, Eduardo Eusebio
Zhang, J.
Zhao, E. G.
author Li, F. X.
author_facet Li, F. X.
Liao, W. P.
Qian, S. B.
Fernandez Lajus, Eduardo Eusebio
Zhang, J.
Zhao, E. G.
author_role author
author2 Liao, W. P.
Qian, S. B.
Fernandez Lajus, Eduardo Eusebio
Zhang, J.
Zhao, E. G.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Multiple stars
Contact binary stars
Eclipsing binary stars
Early stellar evolution
topic Multiple stars
Contact binary stars
Eclipsing binary stars
Early stellar evolution
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv V606 Centauri (V606 Cen) is an early B-type close binary with an orbital period of 1.4950935 days, and its complete light curves are very difficult to observe on the ground. By analyzing the continuous light curve obtained by TESS, we found that it is a marginal contact binary with a very low fill-out factor of about 2%. The O - C diagram of V606 Cen is constructed for the first time based on 118.8 yr of eclipse times. The O - C diagram has been found to show a downward parabolic change together with a cyclic oscillation with a semiamplitude of 0.0545 days and a period of 88.3 yr. The downward parabolic variation reveals a linear period decrease at a rate of dP/dt = -2.08 × 10-7 days yr-1 that can be explained by the mass transfer from the more massive component to the less massive one. Both the marginal contact configuration and the continuous period decrease suggest that V606 Cen is a newly formed contact binary via Case A mass transfer. The cyclic change in the O - C diagram can be explained by the light-travel time effect via the presence of a third body. The lowest mass of the tertiary companion is determined to be M 3 = 4.51 (±0.43) M o˙ and the tertiary is orbiting around the central eclipsing binary in a nearly circular orbit (e = 0.33). All of the results indicate that V606 Cen is a newly formed massive contact binary in a hierarchical triple system.
Fil: Li, F. X.. Chinese Academy of Sciences; República de China. Yunnan Observatories; China. Chinese Academy of Sciences; República de China
Fil: Liao, W. P.. Yunnan Observatories; China. Chinese Academy of Sciences; República de China
Fil: Qian, S. B.. Yunnan Observatories; China. Chinese Academy of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Zhang, J.. Chinese Academy of Sciences; República de China. Yunnan Observatories; China
Fil: Zhao, E. G.. Chinese Academy of Sciences; República de China. Yunnan Observatories; China
description V606 Centauri (V606 Cen) is an early B-type close binary with an orbital period of 1.4950935 days, and its complete light curves are very difficult to observe on the ground. By analyzing the continuous light curve obtained by TESS, we found that it is a marginal contact binary with a very low fill-out factor of about 2%. The O - C diagram of V606 Cen is constructed for the first time based on 118.8 yr of eclipse times. The O - C diagram has been found to show a downward parabolic change together with a cyclic oscillation with a semiamplitude of 0.0545 days and a period of 88.3 yr. The downward parabolic variation reveals a linear period decrease at a rate of dP/dt = -2.08 × 10-7 days yr-1 that can be explained by the mass transfer from the more massive component to the less massive one. Both the marginal contact configuration and the continuous period decrease suggest that V606 Cen is a newly formed contact binary via Case A mass transfer. The cyclic change in the O - C diagram can be explained by the light-travel time effect via the presence of a third body. The lowest mass of the tertiary companion is determined to be M 3 = 4.51 (±0.43) M o˙ and the tertiary is orbiting around the central eclipsing binary in a nearly circular orbit (e = 0.33). All of the results indicate that V606 Cen is a newly formed massive contact binary in a hierarchical triple system.
publishDate 2022
dc.date.none.fl_str_mv 2022-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/211929
Li, F. X.; Liao, W. P.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio; Zhang, J.; et al.; V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System; IOP Publishing; Astrophysical Journal; 924; 1; 1-2022; 1-11
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/211929
identifier_str_mv Li, F. X.; Liao, W. P.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio; Zhang, J.; et al.; V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System; IOP Publishing; Astrophysical Journal; 924; 1; 1-2022; 1-11
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ac3425
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ac3425
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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