Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae

Autores
Benvenuto, Omar Gustavo; Panei, Jorge; Nomoto, Ken'ichi; Kitamura, Hikaru; Hachisu, Izumi
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We study the occurrence of delayed SNe Ia in the single degenerate scenario. We assume that a massive carbon– oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it spin at the critical rate. We assume uniform rotation due to magnetic field coupling. The carbon ignition mass for non-rotating WDs is M_{ig}^NR 1.38≈M_{⨀}, while for the case of uniformly rotating WDs it is a few percent larger (M_{ig}^R 1.43≈M_{⨀}). When accretion rate decreases, the WD begins to lose angular momentum, shrinks, and spins up; however, it does not overflow its critical rotation rate, avoiding mass shedding. Thus, angular momentum losses can lead the CO WD interior to compression and carbon ignition, which would induce an SN Ia. The delay, largely due to the angular momentum losses timescale, may be large enough to allow the companion star to evolve to a He WD, becoming undetectable at the moment of explosion. This scenario supports the occurrence of delayed SNe Ia if the final CO WD mass is 1.38M_{⨀} < M < 1.43 M_{⨀}. We also find that if the delay is longer than ∼3 Gyr, the WD would become too cold to explode, rather undergoing collapse.
Materia
Astronomía
nuclear reactions
stars rotation
supernova
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/4.0/
Repositorio
CIC Digital (CICBA)
Institución
Comisión de Investigaciones Científicas de la Provincia de Buenos Aires
OAI Identificador
oai:digital.cic.gba.gob.ar:11746/4337

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oai_identifier_str oai:digital.cic.gba.gob.ar:11746/4337
network_acronym_str CICBA
repository_id_str 9441
network_name_str CIC Digital (CICBA)
spelling Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia SupernovaeBenvenuto, Omar GustavoPanei, JorgeNomoto, Ken'ichiKitamura, HikaruHachisu, IzumiAstronomíanuclear reactionsstars rotationsupernovaWe study the occurrence of delayed SNe Ia in the single degenerate scenario. We assume that a massive carbon– oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it spin at the critical rate. We assume uniform rotation due to magnetic field coupling. The carbon ignition mass for non-rotating WDs is M_{ig}^NR 1.38≈M_{⨀}, while for the case of uniformly rotating WDs it is a few percent larger (M_{ig}^R 1.43≈M_{⨀}). When accretion rate decreases, the WD begins to lose angular momentum, shrinks, and spins up; however, it does not overflow its critical rotation rate, avoiding mass shedding. Thus, angular momentum losses can lead the CO WD interior to compression and carbon ignition, which would induce an SN Ia. The delay, largely due to the angular momentum losses timescale, may be large enough to allow the companion star to evolve to a He WD, becoming undetectable at the moment of explosion. This scenario supports the occurrence of delayed SNe Ia if the final CO WD mass is 1.38M_{⨀} < M < 1.43 M_{⨀}. We also find that if the delay is longer than ∼3 Gyr, the WD would become too cold to explode, rather undergoing collapse.IOP science2015-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttps://digital.cic.gba.gob.ar/handle/11746/4337enginfo:eu-repo/semantics/altIdentifier/doi/10.1088/2041-8205/809/1/L6info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/reponame:CIC Digital (CICBA)instname:Comisión de Investigaciones Científicas de la Provincia de Buenos Airesinstacron:CICBA2025-09-29T13:39:49Zoai:digital.cic.gba.gob.ar:11746/4337Institucionalhttp://digital.cic.gba.gob.arOrganismo científico-tecnológicoNo correspondehttp://digital.cic.gba.gob.ar/oai/snrdmarisa.degiusti@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:94412025-09-29 13:39:49.554CIC Digital (CICBA) - Comisión de Investigaciones Científicas de la Provincia de Buenos Airesfalse
dc.title.none.fl_str_mv Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
title Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
spellingShingle Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
Benvenuto, Omar Gustavo
Astronomía
nuclear reactions
stars rotation
supernova
title_short Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
title_full Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
title_fullStr Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
title_full_unstemmed Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
title_sort Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
dc.creator.none.fl_str_mv Benvenuto, Omar Gustavo
Panei, Jorge
Nomoto, Ken'ichi
Kitamura, Hikaru
Hachisu, Izumi
author Benvenuto, Omar Gustavo
author_facet Benvenuto, Omar Gustavo
Panei, Jorge
Nomoto, Ken'ichi
Kitamura, Hikaru
Hachisu, Izumi
author_role author
author2 Panei, Jorge
Nomoto, Ken'ichi
Kitamura, Hikaru
Hachisu, Izumi
author2_role author
author
author
author
dc.subject.none.fl_str_mv Astronomía
nuclear reactions
stars rotation
supernova
topic Astronomía
nuclear reactions
stars rotation
supernova
dc.description.none.fl_txt_mv We study the occurrence of delayed SNe Ia in the single degenerate scenario. We assume that a massive carbon– oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it spin at the critical rate. We assume uniform rotation due to magnetic field coupling. The carbon ignition mass for non-rotating WDs is M_{ig}^NR 1.38≈M_{⨀}, while for the case of uniformly rotating WDs it is a few percent larger (M_{ig}^R 1.43≈M_{⨀}). When accretion rate decreases, the WD begins to lose angular momentum, shrinks, and spins up; however, it does not overflow its critical rotation rate, avoiding mass shedding. Thus, angular momentum losses can lead the CO WD interior to compression and carbon ignition, which would induce an SN Ia. The delay, largely due to the angular momentum losses timescale, may be large enough to allow the companion star to evolve to a He WD, becoming undetectable at the moment of explosion. This scenario supports the occurrence of delayed SNe Ia if the final CO WD mass is 1.38M_{⨀} < M < 1.43 M_{⨀}. We also find that if the delay is longer than ∼3 Gyr, the WD would become too cold to explode, rather undergoing collapse.
description We study the occurrence of delayed SNe Ia in the single degenerate scenario. We assume that a massive carbon– oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it spin at the critical rate. We assume uniform rotation due to magnetic field coupling. The carbon ignition mass for non-rotating WDs is M_{ig}^NR 1.38≈M_{⨀}, while for the case of uniformly rotating WDs it is a few percent larger (M_{ig}^R 1.43≈M_{⨀}). When accretion rate decreases, the WD begins to lose angular momentum, shrinks, and spins up; however, it does not overflow its critical rotation rate, avoiding mass shedding. Thus, angular momentum losses can lead the CO WD interior to compression and carbon ignition, which would induce an SN Ia. The delay, largely due to the angular momentum losses timescale, may be large enough to allow the companion star to evolve to a He WD, becoming undetectable at the moment of explosion. This scenario supports the occurrence of delayed SNe Ia if the final CO WD mass is 1.38M_{⨀} < M < 1.43 M_{⨀}. We also find that if the delay is longer than ∼3 Gyr, the WD would become too cold to explode, rather undergoing collapse.
publishDate 2015
dc.date.none.fl_str_mv 2015-08
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 https://digital.cic.gba.gob.ar/handle/11746/4337
url https://digital.cic.gba.gob.ar/handle/11746/4337
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/2041-8205/809/1/L6
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/4.0/
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv IOP science
publisher.none.fl_str_mv IOP science
dc.source.none.fl_str_mv reponame:CIC Digital (CICBA)
instname:Comisión de Investigaciones Científicas de la Provincia de Buenos Aires
instacron:CICBA
reponame_str CIC Digital (CICBA)
collection CIC Digital (CICBA)
instname_str Comisión de Investigaciones Científicas de la Provincia de Buenos Aires
instacron_str CICBA
institution CICBA
repository.name.fl_str_mv CIC Digital (CICBA) - Comisión de Investigaciones Científicas de la Provincia de Buenos Aires
repository.mail.fl_str_mv marisa.degiusti@sedici.unlp.edu.ar
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score 13.070432