Photometric analysis of the eclipsing polar MN Hya
- Autores
- Wang, Qishan; Qian, Sheng-Bang; Han, Zhong-Tao; Zejda, Miloslav; Fernández Lajús, Eduardo Eusebio; Zhu, Li-Ying
- Año de publicación
- 2018
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- As an eclipsing polar with a 3.39 h orbital period, MN Hya was going through a state change when we observed it during 2009-2016. Ten new mid-eclipse times, along with others obtained from literature, allow us to give a new ephemeris. The residuals of a linear fit show that period decreased during the phase of state change, which means angular momentum was lost during this phase. The associated X-ray observation indicates the mass accretion rate was about 3.6 x 10(-9) M(circle dot)yr(-1). The period decrease indicates that at least 60% of mass being transferred from the secondary was lost, maybe in the form of spherically symmetric stellar wind. In the high state, the data show the intensity of flickering reduced when the system had a higher accretion rate, and that flickering sticks out with a primary timescale of about 2 min, which implies the position of the threading point was about 30 white dwarf radii above its surface. The trend of light curves for the system in its high state follows that of the low state for a large fraction of the phase interval from phase 0 to phase 0.4 since, starting at phase 0.4, the cyclotron feature is visible, and the primary intensity hump of the light curves near phase 0.7 when the system is in the high state did not appear on the curve when it was in the low state. Those facts contradict predictions of the two-pole model.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
techniques: photometric
stars: cataclysmic variables: eclipsing polars
stars: individual (MN Hya) - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/3.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/130787
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Photometric analysis of the eclipsing polar MN HyaWang, QishanQian, Sheng-BangHan, Zhong-TaoZejda, MiloslavFernández Lajús, Eduardo EusebioZhu, Li-YingCiencias Astronómicastechniques: photometricstars: cataclysmic variables: eclipsing polarsstars: individual (MN Hya)As an eclipsing polar with a 3.39 h orbital period, MN Hya was going through a state change when we observed it during 2009-2016. Ten new mid-eclipse times, along with others obtained from literature, allow us to give a new ephemeris. The residuals of a linear fit show that period decreased during the phase of state change, which means angular momentum was lost during this phase. The associated X-ray observation indicates the mass accretion rate was about 3.6 x 10(-9) M(circle dot)yr(-1). The period decrease indicates that at least 60% of mass being transferred from the secondary was lost, maybe in the form of spherically symmetric stellar wind. In the high state, the data show the intensity of flickering reduced when the system had a higher accretion rate, and that flickering sticks out with a primary timescale of about 2 min, which implies the position of the threading point was about 30 white dwarf radii above its surface. The trend of light curves for the system in its high state follows that of the low state for a large fraction of the phase interval from phase 0 to phase 0.4 since, starting at phase 0.4, the cyclotron feature is visible, and the primary intensity hump of the light curves near phase 0.7 when the system is in the high state did not appear on the curve when it was in the low state. Those facts contradict predictions of the two-pole model.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2018-07-11info: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/10915/130787enginfo:eu-repo/semantics/altIdentifier/issn/1674-4527info:eu-repo/semantics/altIdentifier/arxiv/1803.11083info:eu-repo/semantics/altIdentifier/doi/10.1088/1674-4527/18/7/75info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/3.0/Creative Commons Attribution 3.0 Unported (CC BY 3.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:31:17Zoai:sedici.unlp.edu.ar:10915/130787Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:31:17.855SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Photometric analysis of the eclipsing polar MN Hya |
title |
Photometric analysis of the eclipsing polar MN Hya |
spellingShingle |
Photometric analysis of the eclipsing polar MN Hya Wang, Qishan Ciencias Astronómicas techniques: photometric stars: cataclysmic variables: eclipsing polars stars: individual (MN Hya) |
title_short |
Photometric analysis of the eclipsing polar MN Hya |
title_full |
Photometric analysis of the eclipsing polar MN Hya |
title_fullStr |
Photometric analysis of the eclipsing polar MN Hya |
title_full_unstemmed |
Photometric analysis of the eclipsing polar MN Hya |
title_sort |
Photometric analysis of the eclipsing polar MN Hya |
dc.creator.none.fl_str_mv |
Wang, Qishan Qian, Sheng-Bang Han, Zhong-Tao Zejda, Miloslav Fernández Lajús, Eduardo Eusebio Zhu, Li-Ying |
author |
Wang, Qishan |
author_facet |
Wang, Qishan Qian, Sheng-Bang Han, Zhong-Tao Zejda, Miloslav Fernández Lajús, Eduardo Eusebio Zhu, Li-Ying |
author_role |
author |
author2 |
Qian, Sheng-Bang Han, Zhong-Tao Zejda, Miloslav Fernández Lajús, Eduardo Eusebio Zhu, Li-Ying |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas techniques: photometric stars: cataclysmic variables: eclipsing polars stars: individual (MN Hya) |
topic |
Ciencias Astronómicas techniques: photometric stars: cataclysmic variables: eclipsing polars stars: individual (MN Hya) |
dc.description.none.fl_txt_mv |
As an eclipsing polar with a 3.39 h orbital period, MN Hya was going through a state change when we observed it during 2009-2016. Ten new mid-eclipse times, along with others obtained from literature, allow us to give a new ephemeris. The residuals of a linear fit show that period decreased during the phase of state change, which means angular momentum was lost during this phase. The associated X-ray observation indicates the mass accretion rate was about 3.6 x 10(-9) M(circle dot)yr(-1). The period decrease indicates that at least 60% of mass being transferred from the secondary was lost, maybe in the form of spherically symmetric stellar wind. In the high state, the data show the intensity of flickering reduced when the system had a higher accretion rate, and that flickering sticks out with a primary timescale of about 2 min, which implies the position of the threading point was about 30 white dwarf radii above its surface. The trend of light curves for the system in its high state follows that of the low state for a large fraction of the phase interval from phase 0 to phase 0.4 since, starting at phase 0.4, the cyclotron feature is visible, and the primary intensity hump of the light curves near phase 0.7 when the system is in the high state did not appear on the curve when it was in the low state. Those facts contradict predictions of the two-pole model. Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
description |
As an eclipsing polar with a 3.39 h orbital period, MN Hya was going through a state change when we observed it during 2009-2016. Ten new mid-eclipse times, along with others obtained from literature, allow us to give a new ephemeris. The residuals of a linear fit show that period decreased during the phase of state change, which means angular momentum was lost during this phase. The associated X-ray observation indicates the mass accretion rate was about 3.6 x 10(-9) M(circle dot)yr(-1). The period decrease indicates that at least 60% of mass being transferred from the secondary was lost, maybe in the form of spherically symmetric stellar wind. In the high state, the data show the intensity of flickering reduced when the system had a higher accretion rate, and that flickering sticks out with a primary timescale of about 2 min, which implies the position of the threading point was about 30 white dwarf radii above its surface. The trend of light curves for the system in its high state follows that of the low state for a large fraction of the phase interval from phase 0 to phase 0.4 since, starting at phase 0.4, the cyclotron feature is visible, and the primary intensity hump of the light curves near phase 0.7 when the system is in the high state did not appear on the curve when it was in the low state. Those facts contradict predictions of the two-pole model. |
publishDate |
2018 |
dc.date.none.fl_str_mv |
2018-07-11 |
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/10915/130787 |
url |
http://sedici.unlp.edu.ar/handle/10915/130787 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/1674-4527 info:eu-repo/semantics/altIdentifier/arxiv/1803.11083 info:eu-repo/semantics/altIdentifier/doi/10.1088/1674-4527/18/7/75 |
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eu_rights_str_mv |
openAccess |
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http://creativecommons.org/licenses/by/3.0/ Creative Commons Attribution 3.0 Unported (CC BY 3.0) |
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