  Despite the significance of type Ia supernovae (SNeIa) in many fields in
astrophysics, SNeIa lack a theoretical explanation. We investigate the
potential contribution to the SNeIa rate from the most common progenitor
channels using the binary population synthesis (BPS) code SeBa. Using SeBa, we
aim constrain binary processes such as the common envelope phase and the
efficiency of mass retention of white dwarf accretion. We find that the
simulated rates are not sufficient to explain the observed rates. Further, we
find that the mass retention efficiency of white dwarf accretion significantly
influences the rates, but does not explain all the differences between
simulated rates from different BPS codes.
