The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind

Autores
Zang, Lei; Qian, Shengbang; Fernández Lajús, Eduardo Eusebio
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
WX Cen is most likely one of the Galactic counterparts of compact binary supersoft X-ray sources as a member of the V Sagittae class, in which mass is transferred from a donor secondary to a massive white dwarf primary via an accretion disk. Based on the photometric observations from the TESS space telescope and AAVSO database, 218 times of light minimum were determined. By collecting all available eclipse timings of WX Cen from the literature together with those newly determined, we constructed an O−C diagram and analyzed the variations in the orbital period of the eclipsing binary. It is confirmed that the orbital period is continuously decreasing and the rate of the change in the orbital period is revised to P = -4.4(4)x10⁻⁷day yr⁻¹ = -0.038(3) s yr⁻¹. The mass of the donor secondary is estimated as Ms ∼ 0.6 Me☉, when the white dwarf mass is MWD ∼ 0.9 M☉ By considering a conservative mass transfer from the secondary to the primary, the orbital period of WX Cen should be increasing, which is opposite to the observed continuous decrease. Therefore, the decrease in the period can be plausibly explained as the result of angular momentum loss (AML) via magnetic wind from the secondary and/or from the accretion disk. The AML causes the donor secondary with a low mass to continually be filling its critical Roche lobe and transferring material to the white dwarf. In this way, the evolution of WX Cen is dominated by the magnetic wind and continuously radiating supersoft X-rays.
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/153026

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/153026
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic WindZang, LeiQian, ShengbangFernández Lajús, Eduardo EusebioCiencias AstronómicasFísicaClose binary starsEclipsing binary starsOrbital evolutionWX Cen is most likely one of the Galactic counterparts of compact binary supersoft X-ray sources as a member of the V Sagittae class, in which mass is transferred from a donor secondary to a massive white dwarf primary via an accretion disk. Based on the photometric observations from the TESS space telescope and AAVSO database, 218 times of light minimum were determined. By collecting all available eclipse timings of WX Cen from the literature together with those newly determined, we constructed an O−C diagram and analyzed the variations in the orbital period of the eclipsing binary. It is confirmed that the orbital period is continuously decreasing and the rate of the change in the orbital period is revised to P = -4.4(4)x10⁻⁷day yr⁻¹ = -0.038(3) s yr⁻¹. The mass of the donor secondary is estimated as Ms ∼ 0.6 Me☉, when the white dwarf mass is MWD ∼ 0.9 M☉ By considering a conservative mass transfer from the secondary to the primary, the orbital period of WX Cen should be increasing, which is opposite to the observed continuous decrease. Therefore, the decrease in the period can be plausibly explained as the result of angular momentum loss (AML) via magnetic wind from the secondary and/or from the accretion disk. The AML causes the donor secondary with a low mass to continually be filling its critical Roche lobe and transferring material to the white dwarf. In this way, the evolution of WX Cen is dominated by the magnetic wind and continuously radiating supersoft X-rays.Instituto de Astrofísica de La Plata2023info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/153026enginfo:eu-repo/semantics/altIdentifier/issn/1538-4357info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/acb52finfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:39:34Zoai:sedici.unlp.edu.ar:10915/153026Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:39:34.416SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
title The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
spellingShingle The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
Zang, Lei
Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
title_short The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
title_full The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
title_fullStr The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
title_full_unstemmed The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
title_sort The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
dc.creator.none.fl_str_mv Zang, Lei
Qian, Shengbang
Fernández Lajús, Eduardo Eusebio
author Zang, Lei
author_facet Zang, Lei
Qian, Shengbang
Fernández Lajús, Eduardo Eusebio
author_role author
author2 Qian, Shengbang
Fernández Lajús, Eduardo Eusebio
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
topic Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
dc.description.none.fl_txt_mv WX Cen is most likely one of the Galactic counterparts of compact binary supersoft X-ray sources as a member of the V Sagittae class, in which mass is transferred from a donor secondary to a massive white dwarf primary via an accretion disk. Based on the photometric observations from the TESS space telescope and AAVSO database, 218 times of light minimum were determined. By collecting all available eclipse timings of WX Cen from the literature together with those newly determined, we constructed an O−C diagram and analyzed the variations in the orbital period of the eclipsing binary. It is confirmed that the orbital period is continuously decreasing and the rate of the change in the orbital period is revised to P = -4.4(4)x10⁻⁷day yr⁻¹ = -0.038(3) s yr⁻¹. The mass of the donor secondary is estimated as Ms ∼ 0.6 Me☉, when the white dwarf mass is MWD ∼ 0.9 M☉ By considering a conservative mass transfer from the secondary to the primary, the orbital period of WX Cen should be increasing, which is opposite to the observed continuous decrease. Therefore, the decrease in the period can be plausibly explained as the result of angular momentum loss (AML) via magnetic wind from the secondary and/or from the accretion disk. The AML causes the donor secondary with a low mass to continually be filling its critical Roche lobe and transferring material to the white dwarf. In this way, the evolution of WX Cen is dominated by the magnetic wind and continuously radiating supersoft X-rays.
Instituto de Astrofísica de La Plata
description WX Cen is most likely one of the Galactic counterparts of compact binary supersoft X-ray sources as a member of the V Sagittae class, in which mass is transferred from a donor secondary to a massive white dwarf primary via an accretion disk. Based on the photometric observations from the TESS space telescope and AAVSO database, 218 times of light minimum were determined. By collecting all available eclipse timings of WX Cen from the literature together with those newly determined, we constructed an O−C diagram and analyzed the variations in the orbital period of the eclipsing binary. It is confirmed that the orbital period is continuously decreasing and the rate of the change in the orbital period is revised to P = -4.4(4)x10⁻⁷day yr⁻¹ = -0.038(3) s yr⁻¹. The mass of the donor secondary is estimated as Ms ∼ 0.6 Me☉, when the white dwarf mass is MWD ∼ 0.9 M☉ By considering a conservative mass transfer from the secondary to the primary, the orbital period of WX Cen should be increasing, which is opposite to the observed continuous decrease. Therefore, the decrease in the period can be plausibly explained as the result of angular momentum loss (AML) via magnetic wind from the secondary and/or from the accretion disk. The AML causes the donor secondary with a low mass to continually be filling its critical Roche lobe and transferring material to the white dwarf. In this way, the evolution of WX Cen is dominated by the magnetic wind and continuously radiating supersoft X-rays.
publishDate 2023
dc.date.none.fl_str_mv 2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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://sedici.unlp.edu.ar/handle/10915/153026
url http://sedici.unlp.edu.ar/handle/10915/153026
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/1538-4357
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/acb52f
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
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reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
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institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
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