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Despite the significance of Type Ia supernovae (SNeIa) in many fields inastrophysics, SNeIa lack a theoretical explanation. The standard scenariosinvolve thermonuclear explosions of carbon/oxygen white dwarfs approaching theChandrasekhar mass; either by accretion from a companion or by a merger of twowhite dwarfs. We investigate the contribution from both channels to the SNIarate with the binary population synthesis (BPS) code SeBa in order to constrainbinary processes such as the mass retention efficiency of WD accretion andcommon envelope evolution. We determine the theoretical rates and delay timedistribution of SNIa progenitors and in particular study how assumptions affectthe predicted rates.

Progenitors of Supernovae Type Ia