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
- Institución
- Comisión de Investigaciones Científicas de la Provincia de Buenos Aires
- OAI Identificador
- oai:digital.cic.gba.gob.ar:11746/4337
Ver los metadatos del registro completo
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oai:digital.cic.gba.gob.ar:11746/4337 |
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repository_id_str |
9441 |
network_name_str |
CIC Digital (CICBA) |
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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 |
_version_ |
1844618578741952512 |
score |
13.070432 |