Supernovae type Ia (SN Ia) represent one of the most interesting astrophysical events observed. A SN Ia explosion at its peak can have luminosity equal to a whole galaxy. We know that they are explosions of carbon-oxygen white dwarfs (CO WD) but we don’t know what their progenitors are. In our work we explore the core-degenerate (CD) scenario in which the progenitor is a product of a merger between a WD and the core of an asymptotic giant branch (AGB) star immediately after the common envelope (CE) phase. We generate a population of stars using a given initial mass function (IMF) and then follow the evolution of the stars that are in binaries. We also introduce a novel approach without using the complicated alpha common envelope prescription. We also don’t make distinction between the CD and the double degenerate (DD) scenario in our calculation. Using a simple population synthesis we come to the conclusion that the combined CD and DD scenarios produce enough systems to match the observed numbers of SNIa and the ratio between SNIa and core collapse supernovae (CC SN). |