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The bulk of p isotopes is created in the 'gamma processes' mainly bysequences of photodisintegrations and beta decays in explosive conditions inType Ia supernovae (SNIa) or in core collapse supernovae (ccSN). Thecontribution of different stellar sources to the observed distribution ofp-nuclei in the Solar System is still under debate. We explore singledegenerate Type Ia supernovae in the framework of two-dimensional SNIadelayed-detonation explosion models. Travaglio et al. (2011, TRV11) discussedthe sensitivity of p-nuclei production to different SNIa models, i.e. delayeddetonations of different strength, deflagrations, and the dependence onselected s-process seed distributions. Here we present a detailed study ofp-process nucleosynthesis occuring in SNIa with s-process seeds at differentmetallicities. Based on the delayed-detonation model DDT-a of TRV11, we analyzethe dependence of p-nucleosynthesis on the s-seed distribution obtained fromdifferent strengths of the 13C-pocket. Using a Galactic chemical evolution code(see Travaglio et al. 2004) we study the contribution of SNIa to the solarstable p-nuclei. We find that explosions of Chandrasekhar-mass singledegenerate systems produce a large amount of p-nuclei in our Galaxy, both inthe range of light (A < 120) and heavy p-nuclei, at almost flat averageproduction factors (within a factor of about 3). We discussed in detailsp-isotopes such as 94Mo with a behavior diverging from the average, which weattribute to uncertainties in the nuclear data or in SNIa modelling.

Testing the role of SNe Ia for Galactic chemical evolution of p-nuclei with 2D models and with s-process seeds at different metallicities