Volume 450, Number 2, May I 2006
|Page(s)||655 - 666|
|Section||Stellar structure and evolution|
|Published online||10 April 2006|
The ignition of thermonuclear flames in type Ia supernovae
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching, Germany e-mail: firstname.lastname@example.org
2 Universität Würzburg, Am Hubland, 97074 Würzburg, Germany e-mail: [luigi;niemeyer]@astro.uni-wuerzburg.de
3 International University Bremen, Campus Ring 1, 28759 Bremen, Germany e-mail: email@example.com
Accepted: 20 December 2005
In the framework of the Chandrasekhar-mass deflagration model for type Ia supernovae (SNe Ia), a persisting free parameter is the initial morphology of the flame front, which is linked to the ignition process in the progenitor white dwarf. Previous analytical models indicate that the thermal runaway is driven by temperature perturbations (“bubbles”) that develop in the white dwarf's convective core. In order to probe the conditions at ignition (diameters, temperatures, and evolutionary timescales), we performed hydrodynamical 2D simulations of buoyant bubbles in white dwarf interiors. Our results show that fragmentation occurring during the bubble rise affects the outcome of the bubble evolution. Possible implications for the ignition process of SNe Ia are discussed.
Key words: supernovae: general / hydrodynamics / methods: numerical / white dwarfs
© ESO, 2006
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.