Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet

Autores
Han, Z. T.; Qian, S. B.; Han, Q. W.; Zang, L.; Soonthornthum, B.; Li, L. J.; Zhu, L. Y.; Liu, W.; Fernandez Lajus, Eduardo Eusebio; Dai, Z. B.; Na, W. W.
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present a timing study of the short-period eclipsing cataclysmic variable (CV) HT Cas. Based on new eclipse times derived from our photometric monitoring and archival optical data, combined with historical timings, spanning ∼42 yr, we detect a secular decrease in the orbital period at a rate of  and a cyclic period wiggle with an amplitude of 79.3 s and a period of 30.28 yr. We find that neither gravitational radiation nor magnetic braking can explain the observed decrease rate, suggesting the presence of additional angular momentum loss (AML). The empirical consequential AML (eCAML) model developed by Schreiber et al. can well match the observed orbital decay in HT Cas, and the physical mechanism for eCAML is most likely attributable to the frictional AML following nova eruptions. As for the cyclic variation, the best explanation is the influence of an unseen companion in orbit around the binary. The derived orbital parameters reveal that the hypothetical third body could be a giant planet with mass of M3 ≃ 14MJup that is moving on a highly eccentric orbit (e = 0.82). Taken together the results of the present study suggest that HT Cas is a unique triple system containing a high-eccentricity giant planet and it has the potential to become an ideal laboratory in which to test models of CV evolution.
Fil: Han, Z. T.. Yuxi Normal University; China
Fil: Qian, S. B.. Chinese Academy of Sciences; República de China
Fil: Han, Q. W.. Chinese Academy of Sciences; República de China
Fil: Zang, L.. Chinese Academy of Sciences; República de China
Fil: Soonthornthum, B.. Chinese Academy of Sciences; República de China
Fil: Li, L. J.. Chinese Academy of Sciences; República de China
Fil: Zhu, L. Y.. Chinese Academy of Sciences; República de China
Fil: Liu, W.. Chinese Academy of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Dai, Z. B.. Chinese Academy of Sciences; República de China
Fil: Na, W. W.. Chinese Academy of Sciences; República de China
Materia
Close binary stars (254)
Eclipsing binary stars (444)
Cataclysmic variable stars (203)
Dwarf novae (418)
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:11336/235638
Acceder
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network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant PlanetHan, Z. T.Qian, S. B.Han, Q. W.Zang, L.Soonthornthum, B.Li, L. J.Zhu, L. Y.Liu, W.Fernandez Lajus, Eduardo EusebioDai, Z. B.Na, W. W.Close binary stars (254)Eclipsing binary stars (444)Cataclysmic variable stars (203)Dwarf novae (418)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a timing study of the short-period eclipsing cataclysmic variable (CV) HT Cas. Based on new eclipse times derived from our photometric monitoring and archival optical data, combined with historical timings, spanning ∼42 yr, we detect a secular decrease in the orbital period at a rate of  and a cyclic period wiggle with an amplitude of 79.3 s and a period of 30.28 yr. We find that neither gravitational radiation nor magnetic braking can explain the observed decrease rate, suggesting the presence of additional angular momentum loss (AML). The empirical consequential AML (eCAML) model developed by Schreiber et al. can well match the observed orbital decay in HT Cas, and the physical mechanism for eCAML is most likely attributable to the frictional AML following nova eruptions. As for the cyclic variation, the best explanation is the influence of an unseen companion in orbit around the binary. The derived orbital parameters reveal that the hypothetical third body could be a giant planet with mass of M3 ≃ 14MJup that is moving on a highly eccentric orbit (e = 0.82). Taken together the results of the present study suggest that HT Cas is a unique triple system containing a high-eccentricity giant planet and it has the potential to become an ideal laboratory in which to test models of CV evolution.Fil: Han, Z. T.. Yuxi Normal University; ChinaFil: Qian, S. B.. Chinese Academy of Sciences; República de ChinaFil: Han, Q. W.. Chinese Academy of Sciences; República de ChinaFil: Zang, L.. Chinese Academy of Sciences; República de ChinaFil: Soonthornthum, B.. Chinese Academy of Sciences; República de ChinaFil: Li, L. J.. Chinese Academy of Sciences; República de ChinaFil: Zhu, L. Y.. Chinese Academy of Sciences; República de ChinaFil: Liu, W.. Chinese Academy of Sciences; República de ChinaFil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Dai, Z. B.. Chinese Academy of Sciences; República de ChinaFil: Na, W. W.. Chinese Academy of Sciences; República de ChinaIOP Publishing2023-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/235638Han, Z. T.; Qian, S. B.; Han, Q. W.; Zang, L.; Soonthornthum, B.; et al.; Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet; IOP Publishing; Astrophysical Journal; 953; 1; 8-2023; 63, 1-120004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/acdd6einfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/acdd6einfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:44:04Zoai:ri.conicet.gov.ar:11336/235638instacron: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 09:44:04.746CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
title Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
spellingShingle Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
Han, Z. T.
Close binary stars (254)
Eclipsing binary stars (444)
Cataclysmic variable stars (203)
Dwarf novae (418)
title_short Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
title_full Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
title_fullStr Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
title_full_unstemmed Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
title_sort Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet
dc.creator.none.fl_str_mv Han, Z. T.
Qian, S. B.
Han, Q. W.
Zang, L.
Soonthornthum, B.
Li, L. J.
Zhu, L. Y.
Liu, W.
Fernandez Lajus, Eduardo Eusebio
Dai, Z. B.
Na, W. W.
author Han, Z. T.
author_facet Han, Z. T.
Qian, S. B.
Han, Q. W.
Zang, L.
Soonthornthum, B.
Li, L. J.
Zhu, L. Y.
Liu, W.
Fernandez Lajus, Eduardo Eusebio
Dai, Z. B.
Na, W. W.
author_role author
author2 Qian, S. B.
Han, Q. W.
Zang, L.
Soonthornthum, B.
Li, L. J.
Zhu, L. Y.
Liu, W.
Fernandez Lajus, Eduardo Eusebio
Dai, Z. B.
Na, W. W.
author2_role author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Close binary stars (254)
Eclipsing binary stars (444)
Cataclysmic variable stars (203)
Dwarf novae (418)
topic Close binary stars (254)
Eclipsing binary stars (444)
Cataclysmic variable stars (203)
Dwarf novae (418)
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present a timing study of the short-period eclipsing cataclysmic variable (CV) HT Cas. Based on new eclipse times derived from our photometric monitoring and archival optical data, combined with historical timings, spanning ∼42 yr, we detect a secular decrease in the orbital period at a rate of  and a cyclic period wiggle with an amplitude of 79.3 s and a period of 30.28 yr. We find that neither gravitational radiation nor magnetic braking can explain the observed decrease rate, suggesting the presence of additional angular momentum loss (AML). The empirical consequential AML (eCAML) model developed by Schreiber et al. can well match the observed orbital decay in HT Cas, and the physical mechanism for eCAML is most likely attributable to the frictional AML following nova eruptions. As for the cyclic variation, the best explanation is the influence of an unseen companion in orbit around the binary. The derived orbital parameters reveal that the hypothetical third body could be a giant planet with mass of M3 ≃ 14MJup that is moving on a highly eccentric orbit (e = 0.82). Taken together the results of the present study suggest that HT Cas is a unique triple system containing a high-eccentricity giant planet and it has the potential to become an ideal laboratory in which to test models of CV evolution.
Fil: Han, Z. T.. Yuxi Normal University; China
Fil: Qian, S. B.. Chinese Academy of Sciences; República de China
Fil: Han, Q. W.. Chinese Academy of Sciences; República de China
Fil: Zang, L.. Chinese Academy of Sciences; República de China
Fil: Soonthornthum, B.. Chinese Academy of Sciences; República de China
Fil: Li, L. J.. Chinese Academy of Sciences; República de China
Fil: Zhu, L. Y.. Chinese Academy of Sciences; República de China
Fil: Liu, W.. Chinese Academy of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Dai, Z. B.. Chinese Academy of Sciences; República de China
Fil: Na, W. W.. Chinese Academy of Sciences; República de China
description We present a timing study of the short-period eclipsing cataclysmic variable (CV) HT Cas. Based on new eclipse times derived from our photometric monitoring and archival optical data, combined with historical timings, spanning ∼42 yr, we detect a secular decrease in the orbital period at a rate of  and a cyclic period wiggle with an amplitude of 79.3 s and a period of 30.28 yr. We find that neither gravitational radiation nor magnetic braking can explain the observed decrease rate, suggesting the presence of additional angular momentum loss (AML). The empirical consequential AML (eCAML) model developed by Schreiber et al. can well match the observed orbital decay in HT Cas, and the physical mechanism for eCAML is most likely attributable to the frictional AML following nova eruptions. As for the cyclic variation, the best explanation is the influence of an unseen companion in orbit around the binary. The derived orbital parameters reveal that the hypothetical third body could be a giant planet with mass of M3 ≃ 14MJup that is moving on a highly eccentric orbit (e = 0.82). Taken together the results of the present study suggest that HT Cas is a unique triple system containing a high-eccentricity giant planet and it has the potential to become an ideal laboratory in which to test models of CV evolution.
publishDate 2023
dc.date.none.fl_str_mv 2023-08
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/11336/235638
Han, Z. T.; Qian, S. B.; Han, Q. W.; Zang, L.; Soonthornthum, B.; et al.; Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet; IOP Publishing; Astrophysical Journal; 953; 1; 8-2023; 63, 1-12
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/235638
identifier_str_mv Han, Z. T.; Qian, S. B.; Han, Q. W.; Zang, L.; Soonthornthum, B.; et al.; Orbital period variations in HT Cas: evidence for additional angular momentum loss and a High-eccentricity Giant Planet; IOP Publishing; Astrophysical Journal; 953; 1; 8-2023; 63, 1-12
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/acdd6e
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/acdd6e
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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