Abstract
In the framework of the Chandrasekar-mass deflagration model for Type Ia supernovae, a persisting free parameter is the initial location 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'') developing in the white dwarf's convective core. In this work, numerical 2D simulations of buoyant bubbles in the white dwarf interior are presented and discussed, in order to probe the bubble features at ignition (diameters, temperatures and evolutionary time scales). The results support the multi-point scenario as the most favored ignition model for the SN Ia explosion.
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