Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph

Autores
Qian, S. B.; Han, Z. T.; Fernandez Lajus, Eduardo Eusebio; Zhu, L. Y.; Li, L. J.; Liao, W. P.; Zhao, E. G.
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
V2051 Oph is a deeply eclipsing dwarf nova with an orbital period below the period gap of cataclysmic variables (CVs). It has been photometrically monitored since 2008 June and 24 mid-eclipse times of the white dwarf have been obtained. The changes in the orbital period are investigated using all of the available mid-eclipse times. A continuous period decrease with a rate of dP/dt = -5.93x10^(-10) days/yr was discovered to be superimposed on a periodic variation with a small amplitude of 0 000329 and a period of 21.64 years. The standard theory predicted that the evolution of CVs below the period gap is driven by gravitational radiation. However, angular momentum loss (AML) via gravitational radiation is insufficient to explain this decrease, and additional AML via magnetic braking that is about five times the gravitational radiation rate is required. This is consistent with the theoretical requirement indicating that magnetic braking of the fully convective star is not completely stopped. The cyclic oscillation was interpreted as the variation of the arriving eclipse time via the presence of a third body because the required energy for the Applegate mechanism is much larger than that radiated from the secondary in 10 years. Its mass is derived as M3 sin i´ = 7.3 (+-0.7) Jupiter mass. For orbital inclinations i >= 30º.3, it would be a planetary object. The giant circumbinary planet is orbiting around V2051 Oph at an orbital separation of about 9.0 astronomical units (AU) in an eccentric orbit (e′ = 0.37). These conclusions support the ideas that some planets could survive stellar late evolution and that dwarf novae are also planetary hosting stars.
Fil: Qian, S. B. . Chinese Academy Of Sciences; República de China
Fil: Han, Z. T. . 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: Zhu, L. Y. . Chinese Academy Of Sciences; República de China
Fil: Li, L. J.. Chinese Academy Of Sciences; República de China
Fil: Liao, W. P. . Chinese Academy Of Sciences; República de China
Fil: Zhao, E. G. . Chinese Academy Of Sciences; República de China
Materia
Eclipsing Binaries
Planetary Systems
Dwarf Nova
Evolution of Stars
V2051 Oph (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:11336/11315
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/11315
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 OphQian, S. B. Han, Z. T. Fernandez Lajus, Eduardo EusebioZhu, L. Y. Li, L. J.Liao, W. P. Zhao, E. G. Eclipsing BinariesPlanetary SystemsDwarf NovaEvolution of StarsV2051 Oph (Estrella)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1V2051 Oph is a deeply eclipsing dwarf nova with an orbital period below the period gap of cataclysmic variables (CVs). It has been photometrically monitored since 2008 June and 24 mid-eclipse times of the white dwarf have been obtained. The changes in the orbital period are investigated using all of the available mid-eclipse times. A continuous period decrease with a rate of dP/dt = -5.93x10^(-10) days/yr was discovered to be superimposed on a periodic variation with a small amplitude of 0 000329 and a period of 21.64 years. The standard theory predicted that the evolution of CVs below the period gap is driven by gravitational radiation. However, angular momentum loss (AML) via gravitational radiation is insufficient to explain this decrease, and additional AML via magnetic braking that is about five times the gravitational radiation rate is required. This is consistent with the theoretical requirement indicating that magnetic braking of the fully convective star is not completely stopped. The cyclic oscillation was interpreted as the variation of the arriving eclipse time via the presence of a third body because the required energy for the Applegate mechanism is much larger than that radiated from the secondary in 10 years. Its mass is derived as M3 sin i´ = 7.3 (+-0.7) Jupiter mass. For orbital inclinations i >= 30º.3, it would be a planetary object. The giant circumbinary planet is orbiting around V2051 Oph at an orbital separation of about 9.0 astronomical units (AU) in an eccentric orbit (e′ = 0.37). These conclusions support the ideas that some planets could survive stellar late evolution and that dwarf novae are also planetary hosting stars.Fil: Qian, S. B. . Chinese Academy Of Sciences; República de ChinaFil: Han, Z. T. . 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: Zhu, L. Y. . Chinese Academy Of Sciences; República de ChinaFil: Li, L. J.. Chinese Academy Of Sciences; República de ChinaFil: Liao, W. P. . Chinese Academy Of Sciences; República de ChinaFil: Zhao, E. G. . Chinese Academy Of Sciences; República de ChinaIop Publishing2015-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/11315Qian, S. B. ; Han, Z. T. ; Fernandez Lajus, Eduardo Eusebio; Zhu, L. Y. ; Li, L. J.; et al.; Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph; Iop Publishing; Astrophysical Journal Supplement Series; 221; 17; 11-2015; 1-70067-0049enginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0067-0049/221/1/17info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0067-0049/221/1/17/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:49:32Zoai:ri.conicet.gov.ar:11336/11315instacron: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 09:49:32.646CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
title Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
spellingShingle Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
Qian, S. B.
Eclipsing Binaries
Planetary Systems
Dwarf Nova
Evolution of Stars
V2051 Oph (Estrella)
title_short Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
title_full Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
title_fullStr Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
title_full_unstemmed Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
title_sort Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph
dc.creator.none.fl_str_mv Qian, S. B.
Han, Z. T.
Fernandez Lajus, Eduardo Eusebio
Zhu, L. Y.
Li, L. J.
Liao, W. P.
Zhao, E. G.
author Qian, S. B.
author_facet Qian, S. B.
Han, Z. T.
Fernandez Lajus, Eduardo Eusebio
Zhu, L. Y.
Li, L. J.
Liao, W. P.
Zhao, E. G.
author_role author
author2 Han, Z. T.
Fernandez Lajus, Eduardo Eusebio
Zhu, L. Y.
Li, L. J.
Liao, W. P.
Zhao, E. G.
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv Eclipsing Binaries
Planetary Systems
Dwarf Nova
Evolution of Stars
V2051 Oph (Estrella)
topic Eclipsing Binaries
Planetary Systems
Dwarf Nova
Evolution of Stars
V2051 Oph (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 V2051 Oph is a deeply eclipsing dwarf nova with an orbital period below the period gap of cataclysmic variables (CVs). It has been photometrically monitored since 2008 June and 24 mid-eclipse times of the white dwarf have been obtained. The changes in the orbital period are investigated using all of the available mid-eclipse times. A continuous period decrease with a rate of dP/dt = -5.93x10^(-10) days/yr was discovered to be superimposed on a periodic variation with a small amplitude of 0 000329 and a period of 21.64 years. The standard theory predicted that the evolution of CVs below the period gap is driven by gravitational radiation. However, angular momentum loss (AML) via gravitational radiation is insufficient to explain this decrease, and additional AML via magnetic braking that is about five times the gravitational radiation rate is required. This is consistent with the theoretical requirement indicating that magnetic braking of the fully convective star is not completely stopped. The cyclic oscillation was interpreted as the variation of the arriving eclipse time via the presence of a third body because the required energy for the Applegate mechanism is much larger than that radiated from the secondary in 10 years. Its mass is derived as M3 sin i´ = 7.3 (+-0.7) Jupiter mass. For orbital inclinations i >= 30º.3, it would be a planetary object. The giant circumbinary planet is orbiting around V2051 Oph at an orbital separation of about 9.0 astronomical units (AU) in an eccentric orbit (e′ = 0.37). These conclusions support the ideas that some planets could survive stellar late evolution and that dwarf novae are also planetary hosting stars.
Fil: Qian, S. B. . Chinese Academy Of Sciences; República de China
Fil: Han, Z. T. . 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: Zhu, L. Y. . Chinese Academy Of Sciences; República de China
Fil: Li, L. J.. Chinese Academy Of Sciences; República de China
Fil: Liao, W. P. . Chinese Academy Of Sciences; República de China
Fil: Zhao, E. G. . Chinese Academy Of Sciences; República de China
description V2051 Oph is a deeply eclipsing dwarf nova with an orbital period below the period gap of cataclysmic variables (CVs). It has been photometrically monitored since 2008 June and 24 mid-eclipse times of the white dwarf have been obtained. The changes in the orbital period are investigated using all of the available mid-eclipse times. A continuous period decrease with a rate of dP/dt = -5.93x10^(-10) days/yr was discovered to be superimposed on a periodic variation with a small amplitude of 0 000329 and a period of 21.64 years. The standard theory predicted that the evolution of CVs below the period gap is driven by gravitational radiation. However, angular momentum loss (AML) via gravitational radiation is insufficient to explain this decrease, and additional AML via magnetic braking that is about five times the gravitational radiation rate is required. This is consistent with the theoretical requirement indicating that magnetic braking of the fully convective star is not completely stopped. The cyclic oscillation was interpreted as the variation of the arriving eclipse time via the presence of a third body because the required energy for the Applegate mechanism is much larger than that radiated from the secondary in 10 years. Its mass is derived as M3 sin i´ = 7.3 (+-0.7) Jupiter mass. For orbital inclinations i >= 30º.3, it would be a planetary object. The giant circumbinary planet is orbiting around V2051 Oph at an orbital separation of about 9.0 astronomical units (AU) in an eccentric orbit (e′ = 0.37). These conclusions support the ideas that some planets could survive stellar late evolution and that dwarf novae are also planetary hosting stars.
publishDate 2015
dc.date.none.fl_str_mv 2015-11
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/11336/11315
Qian, S. B. ; Han, Z. T. ; Fernandez Lajus, Eduardo Eusebio; Zhu, L. Y. ; Li, L. J.; et al.; Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph; Iop Publishing; Astrophysical Journal Supplement Series; 221; 17; 11-2015; 1-7
0067-0049
url http://hdl.handle.net/11336/11315
identifier_str_mv Qian, S. B. ; Han, Z. T. ; Fernandez Lajus, Eduardo Eusebio; Zhu, L. Y. ; Li, L. J.; et al.; Long-term decrease and cyclic variation in the orbital period of the eclipsing dwarf nova V2051 Oph; Iop Publishing; Astrophysical Journal Supplement Series; 221; 17; 11-2015; 1-7
0067-0049
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0067-0049/221/1/17
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0067-0049/221/1/17/meta
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 Publishing
publisher.none.fl_str_mv Iop Publishing
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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