Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario

We argue that the multiple shells of circumstellar material (CSM) and the supernovae (SNe) ejecta interaction with the CSM starting 59 d after the explosion of the Type Ia SN PTF 11kx are best described by a violent prompt merger. In this prompt merger scenario, the common envelope (CE) phase is ter...

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Autores: García-Berro Montilla, Enrique|||0000-0002-1623-5838, Torres Gil, Santiago|||0000-0001-5777-5251, Camacho Díaz, Judit|||0000-0003-2322-2098, Soker, Noam, Kashi, Amit
Tipo de recurso: artículo
Fecha de publicación:2013
País:España
Institución:Universitat Politècnica de Catalunya (UPC)
Repositorio:UPCommons. Portal del coneixement obert de la UPC
Idioma:inglés
OAI Identifier:oai:upcommons.upc.edu:2117/24103
Acceso en línea:https://hdl.handle.net/2117/24103
https://dx.doi.org/10.1093/mnras/stt271
Access Level:acceso abierto
Palabra clave:Supernova remnants
supernovae: general
supernovae: individual: PTF 11kx
Supernoves
Àrees temàtiques de la UPC::Física
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repository_id_str
spelling Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenarioGarcía-Berro Montilla, Enrique|||0000-0002-1623-5838Torres Gil, Santiago|||0000-0001-5777-5251Camacho Díaz, Judit|||0000-0003-2322-2098Soker, NoamKashi, AmitSupernova remnantssupernovae: generalsupernovae: generalsupernovae: individual: PTF 11kxSupernovesÀrees temàtiques de la UPC::FísicaWe argue that the multiple shells of circumstellar material (CSM) and the supernovae (SNe) ejecta interaction with the CSM starting 59 d after the explosion of the Type Ia SN PTF 11kx are best described by a violent prompt merger. In this prompt merger scenario, the common envelope (CE) phase is terminated by a merger of a white dwarf (WD) companion with the hot core of a massive asymptotic giant branch star. In most cases, the WD is disrupted and accreted on to the more massive core. However, in the rare cases, where the merger takes place when the WD is denser than the core, the core will be disrupted and accreted on to the cooler WD. In such cases, the explosion might occur with no appreciable delay, i.e. months to years after the termination of the CE phase. This, we propose, might be the evolutionary route that could lead to the explosion of PTF 11kx. This scenario can account for the very massive CSM within similar to 1000 au of the exploding PTF 11kx star, for the presence of hydrogen, and for the presence of shells in the CSM.Peer Reviewed20132013-05-0120142014-09-18journal articlehttp://purl.org/coar/resource_type/c_6501VoRhttp://purl.org/coar/version/c_970fb48d4fbd8a85info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/2117/24103https://dx.doi.org/10.1093/mnras/stt271reponame:UPCommons. Portal del coneixement obert de la UPCinstname:Universitat Politècnica de Catalunya (UPC)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:upcommons.upc.edu:2117/241032026-05-27T15:37:01Z
dc.title.none.fl_str_mv Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
title Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
spellingShingle Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
García-Berro Montilla, Enrique|||0000-0002-1623-5838
Supernova remnants
supernovae: general
supernovae: general
supernovae: individual: PTF 11kx
Supernoves
Àrees temàtiques de la UPC::Física
title_short Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
title_full Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
title_fullStr Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
title_full_unstemmed Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
title_sort Explaining the Type Ia supernova PTF 11kx with a violent prompt merger scenario
dc.creator.none.fl_str_mv García-Berro Montilla, Enrique|||0000-0002-1623-5838
Torres Gil, Santiago|||0000-0001-5777-5251
Camacho Díaz, Judit|||0000-0003-2322-2098
Soker, Noam
Kashi, Amit
author García-Berro Montilla, Enrique|||0000-0002-1623-5838
author_facet García-Berro Montilla, Enrique|||0000-0002-1623-5838
Torres Gil, Santiago|||0000-0001-5777-5251
Camacho Díaz, Judit|||0000-0003-2322-2098
Soker, Noam
Kashi, Amit
author_role author
author2 Torres Gil, Santiago|||0000-0001-5777-5251
Camacho Díaz, Judit|||0000-0003-2322-2098
Soker, Noam
Kashi, Amit
author2_role author
author
author
author
dc.subject.none.fl_str_mv Supernova remnants
supernovae: general
supernovae: general
supernovae: individual: PTF 11kx
Supernoves
Àrees temàtiques de la UPC::Física
topic Supernova remnants
supernovae: general
supernovae: general
supernovae: individual: PTF 11kx
Supernoves
Àrees temàtiques de la UPC::Física
description We argue that the multiple shells of circumstellar material (CSM) and the supernovae (SNe) ejecta interaction with the CSM starting 59 d after the explosion of the Type Ia SN PTF 11kx are best described by a violent prompt merger. In this prompt merger scenario, the common envelope (CE) phase is terminated by a merger of a white dwarf (WD) companion with the hot core of a massive asymptotic giant branch star. In most cases, the WD is disrupted and accreted on to the more massive core. However, in the rare cases, where the merger takes place when the WD is denser than the core, the core will be disrupted and accreted on to the cooler WD. In such cases, the explosion might occur with no appreciable delay, i.e. months to years after the termination of the CE phase. This, we propose, might be the evolutionary route that could lead to the explosion of PTF 11kx. This scenario can account for the very massive CSM within similar to 1000 au of the exploding PTF 11kx star, for the presence of hydrogen, and for the presence of shells in the CSM.
publishDate 2013
dc.date.none.fl_str_mv 2013
2013-05-01
2014
2014-09-18
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
VoR
http://purl.org/coar/version/c_970fb48d4fbd8a85
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/2117/24103
https://dx.doi.org/10.1093/mnras/stt271
url https://hdl.handle.net/2117/24103
https://dx.doi.org/10.1093/mnras/stt271
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
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
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:UPCommons. Portal del coneixement obert de la UPC
instname:Universitat Politècnica de Catalunya (UPC)
instname_str Universitat Politècnica de Catalunya (UPC)
reponame_str UPCommons. Portal del coneixement obert de la UPC
collection UPCommons. Portal del coneixement obert de la UPC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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