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

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...

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Autores principales: Zang, Lei, Qian, Shengbang, Fernández Lajús, Eduardo Eusebio
Formato: Articulo
Lenguaje:Inglés
Publicado: 2023
Materias:
Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/153026
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-153026
record_format dspace
spelling I19-R120-10915-1530262023-05-16T04:03:28Z http://sedici.unlp.edu.ar/handle/10915/153026 issn:1538-4357 The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind Zang, Lei Qian, Shengbang Fernández Lajús, Eduardo Eusebio 2023 2023-05-15T18:39:15Z en Ciencias Astronómicas Física Close binary stars Eclipsing binary stars Orbital evolution 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 Articulo Articulo http://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International (CC BY 4.0) application/pdf
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
spellingShingle Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
Zang, Lei
Qian, Shengbang
Fernández Lajús, Eduardo Eusebio
The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
topic_facet Ciencias Astronómicas
Física
Close binary stars
Eclipsing binary stars
Orbital evolution
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.
format Articulo
Articulo
author Zang, Lei
Qian, Shengbang
Fernández Lajús, Eduardo Eusebio
author_facet Zang, Lei
Qian, Shengbang
Fernández Lajús, Eduardo Eusebio
author_sort Zang, Lei
title The Evolution of the Supersoft X-Ray Source WX Cen Dominated by Magnetic Wind
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 evolution of the supersoft x-ray source wx cen dominated by magnetic wind
publishDate 2023
url http://sedici.unlp.edu.ar/handle/10915/153026
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