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

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. The carbon i...

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Detalles Bibliográficos
Autores principales: Benvenuto, Omar Gustavo, Panei, Jorge Alejandro, Nomoto, Ken'ichi, Kitamura, Hikaru, Hachisu, Izumi
Formato: Articulo
Lenguaje:Inglés
Publicado: 2015
Materias:
Astronomía
binaries: close
nuclear reactions, nucleosynthesis, abundances
stars: rotation
supernovae: general
white dwarfs
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/127319
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-127319
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Astronomía
binaries: close
nuclear reactions, nucleosynthesis, abundances
stars: rotation
supernovae: general
white dwarfs
spellingShingle Astronomía
binaries: close
nuclear reactions, nucleosynthesis, abundances
stars: rotation
supernovae: general
white dwarfs
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
topic_facet Astronomía
binaries: close
nuclear reactions, nucleosynthesis, abundances
stars: rotation
supernovae: general
white dwarfs
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. The carbon ignition mass for non-rotating WDs is M<sub>ig</sub><sup>NR</sup> ≈ 1.38 M⊙; while for the case of uniformly rotating WDs it is a few percent larger (M<sub>ig</sub><sup>R</sup> ≈ 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 M⊙ < 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.
format Articulo
Articulo
author Benvenuto, Omar Gustavo
Panei, Jorge Alejandro
Nomoto, Ken'ichi
Kitamura, Hikaru
Hachisu, Izumi
author_facet Benvenuto, Omar Gustavo
Panei, Jorge Alejandro
Nomoto, Ken'ichi
Kitamura, Hikaru
Hachisu, Izumi
author_sort Benvenuto, Omar Gustavo
title Final Evolution and Delayed Explosions of Spinning White Dwarfs in Single Degenerate Models for Type Ia Supernovae
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
publishDate 2015
url http://sedici.unlp.edu.ar/handle/10915/127319
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