Type Ia Supernova models arising from different distributions of igniting points

In this paper we address the theory of Type Ia supernovae from the moment of carbon runaway up to several hours after the explosion. We have concentrated on the boiling-pot model: a deflagration characterized by the (nearly-) simultaneous ignition of a number of bubbles that pervade the core of the white dwarf. Thermal fluctuations larger than >1% of the background temperature (7x10^8 K) on lengthscales of 3-4 per octant), the explosion produces about 0.45 solar masses of 56Ni, and the kinetic energy of the ejecta is 0.45x10^{51} ergs. However, all three-dimensional deflagration models share three main drawbacks: 1) the scarce synthesis of intermediate-mass elements, 2) the loss of chemical stratification of the ejecta due to mixing by Rayleigh-Taylor instabilities during the first second of the explosion, and 3) the presence of big clumps of 56Ni at the photosphere at the time of maximum brightness