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Using a population number synthesis code with detailed binary evolution, wecalculate the distribution of the number of type Ia supernovae as a function oftime after starburst. This is done for both main progenitor scenarios (singledegenerate and double degenerate), but also with various evolutionaryassumptions (such as mass transfer efficiency, angular momentum loss, andcommon envelope description). The comparison of these theoretically predicteddelay time distributions with observations in elliptical galaxies then allowsto constrain the evolutionary scenarios and parameters. From the morphologicalshape of the distributions, we conclude that all supernovae Ia cannot beproduced through the single degenerate scenario alone, with the best matchbeing obtained when both scenarios contribute. Within the double degeneratescenario, most systems go through a phase of quasi-conservative, stable Rochelobe overflow. We propose stellar rotation as a possible solution for theunderestimation of the observed absolute number of events, as is the case inmany theoretical population synthesis studies. A brief comparison with theseother studies is made, showing good correspondence under the nontrivialcondition of equivalent assumptions. We also investigate the influence ofdifferent supernova Ia progenitors and evolutionary parameters on thetheoretical distribution of the iron abundance of G-type dwarfs in the Galacticdisk. These stars are good indicators of the entire chemical history of theGalaxy, and their predicted metallicity distribution can also be compared tothe observational ones. This again limits the number of acceptable combinationsof assumptions. Supporting previous results, the best correspondence is foundin the case where both the single and double degenerate scenario contribute.

Two distributions shedding light on supernova Ia progenitors: delay times and G-dwarf metallicities