TESTING THE ROLE OF SNe Ia FOR GALACTIC CHEMICAL EVOLUTION OF p -NUCLEI WITH TWO-DIMENSIONAL MODELS AND WITH s -PROCESS SEEDS AT DIFFERENT METALLICITIES

The bulk of p isotopes is created in the "gamma processes" mainly by sequences of photo-dis-integrations and beta decays in explosive conditions in Type Ia supernovae (SNIa) or in core collapse supernovae (ccSN). The contribution of different stellar sources to the observed distribution of p-nuclei in the solar system is still under debate. We explore single degenerate Type Ia supernovae in the framework of two-dimensional SNIa delayed-detonation explosion models. Travaglio et al. discussed the sensitivity of p-nuclei production to different SNIa models, i.e., delayed detonations of different strength, deflagrations, and the dependence on selected s-process seed distributions. We discussed in details p-isotopes such as [sup 94]Mo with a behavior diverging from the average, which we attribute to uncertainties in the nuclear data or in SNIa modeling. If these are explained in the framework of explosions of Chandrasekhar-mass white dwarfs resulting from the single-degenerate progenitor channel, we find that they are responsible for at least 50% of the p-nuclei abundances in the solar system.