Final evolution and delayed explosions of spinning white dwarfs in single degenerate models for type Ia supernovae

Autores
Benvenuto, Omar Gustavo; Panei, Jorge Alejandro; 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 (SD) scenario. We assume that a massive carbon-oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it to spin at the critical rate. We assume uniform rotation due to magnetic field coupling.NR The carbon ignition mass for non-rotating WDs is M ig ≈ 1.38 M ⊙ ; while for the case of uniformly R rotating WDs it is a few percent larger (M ig ≈ 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 1.38 Msun < M < 1.43 Msun . We also find that if the delay is longer than ∼ 3 Gyr, the WD would become too cold to explode, rather undergoing collapse.
Fil: Benvenuto, Omar Gustavo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina
Fil: Panei, Jorge Alejandro. 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: Nomoto, Ken’ichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón
Fil: Kitamura, Hikaru. Kyoto University. Department of Physics; Japón
Fil: Hachisu, Izumi. The University of Tokyo; Japón
Materia
Close Binaries
Supernovae
Nuclear Reactions
Nucleosynthesis
Abundances
Star Rotation
White Dwarfs
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:11336/12613
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/12613
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Final evolution and delayed explosions of spinning white dwarfs in single degenerate models for type Ia supernovaeBenvenuto, Omar GustavoPanei, Jorge AlejandroNomoto, Ken’ichi Kitamura, HikaruHachisu, IzumiClose BinariesSupernovaeNuclear ReactionsNucleosynthesisAbundancesStar RotationWhite Dwarfshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We study the occurrence of delayed SNe Ia in the single degenerate (SD) scenario. We assume that a massive carbon-oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it to spin at the critical rate. We assume uniform rotation due to magnetic field coupling.NR The carbon ignition mass for non-rotating WDs is M ig ≈ 1.38 M ⊙ ; while for the case of uniformly R rotating WDs it is a few percent larger (M ig ≈ 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 1.38 Msun < M < 1.43 Msun . We also find that if the delay is longer than ∼ 3 Gyr, the WD would become too cold to explode, rather undergoing collapse.Fil: Benvenuto, Omar Gustavo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; ArgentinaFil: Panei, Jorge Alejandro. 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: Nomoto, Ken’ichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; JapónFil: Kitamura, Hikaru. Kyoto University. Department of Physics; JapónFil: Hachisu, Izumi. The University of Tokyo; JapónIop Publishing2015-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/12613Benvenuto, Omar Gustavo; Panei, Jorge Alejandro; Nomoto, Ken’ichi ; Kitamura, Hikaru; Hachisu, Izumi; Final evolution and delayed explosions of spinning white dwarfs in single degenerate models for type Ia supernovae; Iop Publishing; Astrophysical Journal; 809; L6; 8-2015; 6-100004-637Xenginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/2041-8205/809/1/L6/metainfo:eu-repo/semantics/altIdentifier/doi/10.1088/2041-8205/809/1/L6info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:39:27Zoai:ri.conicet.gov.ar:11336/12613instacron: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:34982025-09-29 10:39:27.505CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
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
Close Binaries
Supernovae
Nuclear Reactions
Nucleosynthesis
Abundances
Star Rotation
White Dwarfs
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 Alejandro
Nomoto, Ken’ichi
Kitamura, Hikaru
Hachisu, Izumi
author Benvenuto, Omar Gustavo
author_facet Benvenuto, Omar Gustavo
Panei, Jorge Alejandro
Nomoto, Ken’ichi
Kitamura, Hikaru
Hachisu, Izumi
author_role author
author2 Panei, Jorge Alejandro
Nomoto, Ken’ichi
Kitamura, Hikaru
Hachisu, Izumi
author2_role author
author
author
author
dc.subject.none.fl_str_mv Close Binaries
Supernovae
Nuclear Reactions
Nucleosynthesis
Abundances
Star Rotation
White Dwarfs
topic Close Binaries
Supernovae
Nuclear Reactions
Nucleosynthesis
Abundances
Star Rotation
White Dwarfs
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 study the occurrence of delayed SNe Ia in the single degenerate (SD) scenario. We assume that a massive carbon-oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it to spin at the critical rate. We assume uniform rotation due to magnetic field coupling.NR The carbon ignition mass for non-rotating WDs is M ig ≈ 1.38 M ⊙ ; while for the case of uniformly R rotating WDs it is a few percent larger (M ig ≈ 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 1.38 Msun < M < 1.43 Msun . We also find that if the delay is longer than ∼ 3 Gyr, the WD would become too cold to explode, rather undergoing collapse.
Fil: Benvenuto, Omar Gustavo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina
Fil: Panei, Jorge Alejandro. 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: Nomoto, Ken’ichi . University of Tokyo. Kavli Institute for the Physics and Mathematics of the Universe; Japón
Fil: Kitamura, Hikaru. Kyoto University. Department of Physics; Japón
Fil: Hachisu, Izumi. The University of Tokyo; Japón
description We study the occurrence of delayed SNe Ia in the single degenerate (SD) scenario. We assume that a massive carbon-oxygen (CO) white dwarf (WD) accretes matter coming from a companion star, making it to spin at the critical rate. We assume uniform rotation due to magnetic field coupling.NR The carbon ignition mass for non-rotating WDs is M ig ≈ 1.38 M ⊙ ; while for the case of uniformly R rotating WDs it is a few percent larger (M ig ≈ 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 1.38 Msun < M < 1.43 Msun . 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 http://hdl.handle.net/11336/12613
Benvenuto, Omar Gustavo; Panei, Jorge Alejandro; Nomoto, Ken’ichi ; Kitamura, Hikaru; Hachisu, Izumi; Final evolution and delayed explosions of spinning white dwarfs in single degenerate models for type Ia supernovae; Iop Publishing; Astrophysical Journal; 809; L6; 8-2015; 6-10
0004-637X
url http://hdl.handle.net/11336/12613
identifier_str_mv Benvenuto, Omar Gustavo; Panei, Jorge Alejandro; Nomoto, Ken’ichi ; Kitamura, Hikaru; Hachisu, Izumi; Final evolution and delayed explosions of spinning white dwarfs in single degenerate models for type Ia supernovae; Iop Publishing; Astrophysical Journal; 809; L6; 8-2015; 6-10
0004-637X
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/2041-8205/809/1/L6/meta
info:eu-repo/semantics/altIdentifier/doi/10.1088/2041-8205/809/1/L6
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 13.070432

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