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
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/130787

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network_name_str SEDICI (UNLP)
spelling 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
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/3.0/
Creative Commons Attribution 3.0 Unported (CC BY 3.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/3.0/
Creative Commons Attribution 3.0 Unported (CC BY 3.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
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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
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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