Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?

Autores
Qian, S. B.; Shi, G.; Fernandez Lajus, Eduardo Eusebio; Di Sisto, Romina Paula; Zhu, L. Y.; Liu, L.; Zhao, E. G.; Li, L. J.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
WX Cen is one of a few compact binary supersoft X-ray sources (CBSS) in the Galaxy that is a possible Type Ia supernova (SN Ia) progenitor. The supersoft X-ray radiation is explained as hydrostatic nuclear burning on the surface of the white dwarf component that is accreting hydrogen from a stellar companion at a high rate. If the mass donor in this system has a low mass, as has been suggested in the literature, one would expect a high wind-driven mass transfer rate. In that case, the orbital period of the system should increase. To test this theoretical prediction, we have monitored the system photometrically since 2010. By using four newly determined eclipse timings together with those collected from the literature, we discovered that the orbital period is decreasing at a rate of dP/dt = -5.15×10^-7 days yr-1. The long-term decrease in the orbital period is contrary to the prediction that the system is powered by wind-driven accretion. It therefore seems plausible that the mass donor could be more massive than the white dwarf, and that the mass transfer is driven by the thermal instability of the donor star. This finding suggests that WX Cen is a key object to check the physical mechanisms of mass accretion in CBSS. The corresponding timescale of the period change is about P/dP ~ 0.81 × 106 yr, indicating that WX Cen may evolve into an SNe Ia within one million years in the Galaxy.
Fil: Qian, S. B.. Chinese Academy Of Sciences; República de China
Fil: Shi, G.. Chinese Academy Of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Di Sisto, Romina Paula. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina
Fil: Zhu, L. Y.. Chinese Academy Of Sciences; República de China
Fil: Liu, L.. Chinese Academy Of Sciences; República de China
Fil: Zhao, E. G.. Chinese Academy Of Sciences; República de China
Fil: Li, L. J.. Chinese Academy Of Sciences; República de China
Materia
Close Binaries
Eclipsing Binaries
Evolution of Stars
Wx Cen (Estrella)
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:11336/10662
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/10662
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?Qian, S. B.Shi, G.Fernandez Lajus, Eduardo EusebioDi Sisto, Romina PaulaZhu, L. Y.Liu, L.Zhao, E. G.Li, L. J.Close BinariesEclipsing BinariesEvolution of StarsWx Cen (Estrella)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1WX Cen is one of a few compact binary supersoft X-ray sources (CBSS) in the Galaxy that is a possible Type Ia supernova (SN Ia) progenitor. The supersoft X-ray radiation is explained as hydrostatic nuclear burning on the surface of the white dwarf component that is accreting hydrogen from a stellar companion at a high rate. If the mass donor in this system has a low mass, as has been suggested in the literature, one would expect a high wind-driven mass transfer rate. In that case, the orbital period of the system should increase. To test this theoretical prediction, we have monitored the system photometrically since 2010. By using four newly determined eclipse timings together with those collected from the literature, we discovered that the orbital period is decreasing at a rate of dP/dt = -5.15×10^-7 days yr-1. The long-term decrease in the orbital period is contrary to the prediction that the system is powered by wind-driven accretion. It therefore seems plausible that the mass donor could be more massive than the white dwarf, and that the mass transfer is driven by the thermal instability of the donor star. This finding suggests that WX Cen is a key object to check the physical mechanisms of mass accretion in CBSS. The corresponding timescale of the period change is about P/dP ~ 0.81 × 106 yr, indicating that WX Cen may evolve into an SNe Ia within one million years in the Galaxy.Fil: Qian, S. B.. Chinese Academy Of Sciences; República de ChinaFil: Shi, G.. Chinese Academy Of Sciences; República de ChinaFil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Di Sisto, Romina Paula. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; ArgentinaFil: Zhu, L. Y.. Chinese Academy Of Sciences; República de ChinaFil: Liu, L.. Chinese Academy Of Sciences; República de ChinaFil: Zhao, E. G.. Chinese Academy Of Sciences; República de ChinaFil: Li, L. J.. Chinese Academy Of Sciences; República de ChinaIOP Science2013-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/10662Qian, S. B.; Shi, G.; Fernandez Lajus, Eduardo Eusebio; Di Sisto, Romina Paula; Zhu, L. Y.; et al.; Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?; IOP Science; The Astrohpysical Journal Letters; 771; 2; 8-2013; 1-42041-8205enginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/2041-8205/772/2/L18/info:eu-repo/semantics/altIdentifier/url/http://dx.doi.org/10.1088/2041-8205/772/2/L18info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:53:28Zoai:ri.conicet.gov.ar:11336/10662instacron: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:34982025-09-03 09:53:29.069CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
title Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
spellingShingle Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
Qian, S. B.
Close Binaries
Eclipsing Binaries
Evolution of Stars
Wx Cen (Estrella)
title_short Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
title_full Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
title_fullStr Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
title_full_unstemmed Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
title_sort Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?
dc.creator.none.fl_str_mv Qian, S. B.
Shi, G.
Fernandez Lajus, Eduardo Eusebio
Di Sisto, Romina Paula
Zhu, L. Y.
Liu, L.
Zhao, E. G.
Li, L. J.
author Qian, S. B.
author_facet Qian, S. B.
Shi, G.
Fernandez Lajus, Eduardo Eusebio
Di Sisto, Romina Paula
Zhu, L. Y.
Liu, L.
Zhao, E. G.
Li, L. J.
author_role author
author2 Shi, G.
Fernandez Lajus, Eduardo Eusebio
Di Sisto, Romina Paula
Zhu, L. Y.
Liu, L.
Zhao, E. G.
Li, L. J.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Close Binaries
Eclipsing Binaries
Evolution of Stars
Wx Cen (Estrella)
topic Close Binaries
Eclipsing Binaries
Evolution of Stars
Wx Cen (Estrella)
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv WX Cen is one of a few compact binary supersoft X-ray sources (CBSS) in the Galaxy that is a possible Type Ia supernova (SN Ia) progenitor. The supersoft X-ray radiation is explained as hydrostatic nuclear burning on the surface of the white dwarf component that is accreting hydrogen from a stellar companion at a high rate. If the mass donor in this system has a low mass, as has been suggested in the literature, one would expect a high wind-driven mass transfer rate. In that case, the orbital period of the system should increase. To test this theoretical prediction, we have monitored the system photometrically since 2010. By using four newly determined eclipse timings together with those collected from the literature, we discovered that the orbital period is decreasing at a rate of dP/dt = -5.15×10^-7 days yr-1. The long-term decrease in the orbital period is contrary to the prediction that the system is powered by wind-driven accretion. It therefore seems plausible that the mass donor could be more massive than the white dwarf, and that the mass transfer is driven by the thermal instability of the donor star. This finding suggests that WX Cen is a key object to check the physical mechanisms of mass accretion in CBSS. The corresponding timescale of the period change is about P/dP ~ 0.81 × 106 yr, indicating that WX Cen may evolve into an SNe Ia within one million years in the Galaxy.
Fil: Qian, S. B.. Chinese Academy Of Sciences; República de China
Fil: Shi, G.. Chinese Academy Of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Di Sisto, Romina Paula. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina
Fil: Zhu, L. Y.. Chinese Academy Of Sciences; República de China
Fil: Liu, L.. Chinese Academy Of Sciences; República de China
Fil: Zhao, E. G.. Chinese Academy Of Sciences; República de China
Fil: Li, L. J.. Chinese Academy Of Sciences; República de China
description WX Cen is one of a few compact binary supersoft X-ray sources (CBSS) in the Galaxy that is a possible Type Ia supernova (SN Ia) progenitor. The supersoft X-ray radiation is explained as hydrostatic nuclear burning on the surface of the white dwarf component that is accreting hydrogen from a stellar companion at a high rate. If the mass donor in this system has a low mass, as has been suggested in the literature, one would expect a high wind-driven mass transfer rate. In that case, the orbital period of the system should increase. To test this theoretical prediction, we have monitored the system photometrically since 2010. By using four newly determined eclipse timings together with those collected from the literature, we discovered that the orbital period is decreasing at a rate of dP/dt = -5.15×10^-7 days yr-1. The long-term decrease in the orbital period is contrary to the prediction that the system is powered by wind-driven accretion. It therefore seems plausible that the mass donor could be more massive than the white dwarf, and that the mass transfer is driven by the thermal instability of the donor star. This finding suggests that WX Cen is a key object to check the physical mechanisms of mass accretion in CBSS. The corresponding timescale of the period change is about P/dP ~ 0.81 × 106 yr, indicating that WX Cen may evolve into an SNe Ia within one million years in the Galaxy.
publishDate 2013
dc.date.none.fl_str_mv 2013-08
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/11336/10662
Qian, S. B.; Shi, G.; Fernandez Lajus, Eduardo Eusebio; Di Sisto, Romina Paula; Zhu, L. Y.; et al.; Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?; IOP Science; The Astrohpysical Journal Letters; 771; 2; 8-2013; 1-4
2041-8205
url http://hdl.handle.net/11336/10662
identifier_str_mv Qian, S. B.; Shi, G.; Fernandez Lajus, Eduardo Eusebio; Di Sisto, Romina Paula; Zhu, L. Y.; et al.; Is WX Cen a possible type Ia supernova progenitor with wind-driven mass transfer?; IOP Science; The Astrohpysical Journal Letters; 771; 2; 8-2013; 1-4
2041-8205
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/2041-8205/772/2/L18/
info:eu-repo/semantics/altIdentifier/url/http://dx.doi.org/10.1088/2041-8205/772/2/L18
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 Science
publisher.none.fl_str_mv IOP Science
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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score 13.13397

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