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
• Materia: Astronomía; binaries: close; nuclear reactions, nucleosynthesis, abundances; stars: rotation; supernovae: general; white dwarfs
• Institución: Universidad Nacional de La Plata

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_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 1.38 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.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata