Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn

We report the discovery and characterization of a deeply eclipsingAMCVn-system, Gaia14aae (=ASSASN-14cn). Gaia14aae was identified independently by the All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al.) and by the Gaia Science Alerts project, during two separate outbursts. A third out...

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Detalles Bibliográficos
Autores: Campbell, H. C., Miguel Agustino, Enrique de
Tipo de recurso: artículo
Fecha de publicación:2015
País:España
Institución:Universidad de Huelva (UHU)
Repositorio:Arias Montano. Repositorio Institucional de la Universidad de Huelva
Idioma:inglés
OAI Identifier:oai:ariasmontano.uhu.es:10272/11269
Acceso en línea:http://hdl.handle.net/10272/11269
Access Level:acceso abierto
Palabra clave:Binaries: eclipsing
Novae, cataclysmic variables
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spelling Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cnCampbell, H. C.Miguel Agustino, Enrique deBinaries: eclipsingNovae, cataclysmic variablesWe report the discovery and characterization of a deeply eclipsingAMCVn-system, Gaia14aae (=ASSASN-14cn). Gaia14aae was identified independently by the All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al.) and by the Gaia Science Alerts project, during two separate outbursts. A third outburst is seen in archival Pan-STARRS-1 (PS1; Schlafly et al.; Tonry et al.; Magnier et al.) and ASAS-SN data. Spectroscopy reveals a hot, hydrogen-deficient spectrum with clear double-peaked emission lines, consistent with an accreting double-degenerate classification.We use follow-up photometry to constrain the orbital parameters of the system. We find an orbital period of 49.71 min, which places Gaia14aae at the long period extremum of the outbursting AM CVn period distribution. Gaia14aae is dominated by the light from its accreting white dwarf (WD). Assuming an orbital inclination of 90◦ for the binary system, the contact phases of the WD lead to lower limits of 0.78 and 0.015M on the masses of the accretor and donor, respectively, and a lower limit on the mass ratio of 0.019. Gaia14aae is only the third eclipsingAMCVn star known, and the first in which the WD is totally eclipsed. Using a helium WD model, we estimate the accretor’s effective temperature to be 12 900 ± 200 K. The three outburst events occurred within four months of each other, while no other outburst activity is seen in the previous 8 yr of Catalina Real-time Transient Survey (CRTS; Drake et al.), Pan-STARRS-1 and ASAS-SN data. This suggests that these events might be rebrightenings of the first outburst rather than individual events.Oxford University Press20152015-01-0120152015-01-01journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10272/11269reponame:Arias Montano. Repositorio Institucional de la Universidad de Huelvainstname:Universidad de Huelva (UHU)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Atribución-NoComercial-SinDerivadas 3.0 Españahttp://creativecommons.org/licenses/by-nc-nd/3.0/es/info:eu-repo/semantics/openAccessoai:ariasmontano.uhu.es:10272/112692026-06-02T14:58:11Z
dc.title.none.fl_str_mv Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
title Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
spellingShingle Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
Campbell, H. C.
Binaries: eclipsing
Novae, cataclysmic variables
title_short Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
title_full Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
title_fullStr Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
title_full_unstemmed Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
title_sort Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn
dc.creator.none.fl_str_mv Campbell, H. C.
Miguel Agustino, Enrique de
author Campbell, H. C.
author_facet Campbell, H. C.
Miguel Agustino, Enrique de
author_role author
author2 Miguel Agustino, Enrique de
author2_role author
dc.contributor.none.fl_str_mv
dc.subject.none.fl_str_mv Binaries: eclipsing
Novae, cataclysmic variables
topic Binaries: eclipsing
Novae, cataclysmic variables
description We report the discovery and characterization of a deeply eclipsingAMCVn-system, Gaia14aae (=ASSASN-14cn). Gaia14aae was identified independently by the All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al.) and by the Gaia Science Alerts project, during two separate outbursts. A third outburst is seen in archival Pan-STARRS-1 (PS1; Schlafly et al.; Tonry et al.; Magnier et al.) and ASAS-SN data. Spectroscopy reveals a hot, hydrogen-deficient spectrum with clear double-peaked emission lines, consistent with an accreting double-degenerate classification.We use follow-up photometry to constrain the orbital parameters of the system. We find an orbital period of 49.71 min, which places Gaia14aae at the long period extremum of the outbursting AM CVn period distribution. Gaia14aae is dominated by the light from its accreting white dwarf (WD). Assuming an orbital inclination of 90◦ for the binary system, the contact phases of the WD lead to lower limits of 0.78 and 0.015M on the masses of the accretor and donor, respectively, and a lower limit on the mass ratio of 0.019. Gaia14aae is only the third eclipsingAMCVn star known, and the first in which the WD is totally eclipsed. Using a helium WD model, we estimate the accretor’s effective temperature to be 12 900 ± 200 K. The three outburst events occurred within four months of each other, while no other outburst activity is seen in the previous 8 yr of Catalina Real-time Transient Survey (CRTS; Drake et al.), Pan-STARRS-1 and ASAS-SN data. This suggests that these events might be rebrightenings of the first outburst rather than individual events.
publishDate 2015
dc.date.none.fl_str_mv 2015
2015-01-01
2015
2015-01-01
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv http://hdl.handle.net/10272/11269
url http://hdl.handle.net/10272/11269
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Atribución-NoComercial-SinDerivadas 3.0 España
http://creativecommons.org/licenses/by-nc-nd/3.0/es/
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
Atribución-NoComercial-SinDerivadas 3.0 España
http://creativecommons.org/licenses/by-nc-nd/3.0/es/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:Arias Montano. Repositorio Institucional de la Universidad de Huelva
instname:Universidad de Huelva (UHU)
instname_str Universidad de Huelva (UHU)
reponame_str Arias Montano. Repositorio Institucional de la Universidad de Huelva
collection Arias Montano. Repositorio Institucional de la Universidad de Huelva
repository.name.fl_str_mv
repository.mail.fl_str_mv
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