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The nucleosynthesis of proton-rich isotopes is calculated formulti-dimensional Chandrasekhar-mass models of Type Ia supernovae withdifferent metallicities. The predicted abundances of the short-livedradioactive isotopes 92Nb, 97Tc, 98Tc and 146Sm are given in this framework.The abundance seeds are obtained by calculating s-process nucleosynthesis inthe material accreted onto a carbon-oxygen white dwarf from a binary companion.A fine grid of s-seeds at different metallicities and 13C-pocket efficienciesis considered. A galactic chemical evolution model is used to predict thecontribution of SNIa to the solar system p-nuclei composition measured inmeteorites. Nuclear physics uncertainties are critical to determine the role ofSNeIa in the production of 92Nb and 146Sm. We find that, if standardChandrasekhar-mass SNeIa are at least 50% of all SNIa, they are strongcandidates for reproducing the radiogenic p-process signature observed inmeteorites.

Radiogenic p-isotopes from SNIa, nuclear physics uncertainties and Galactic chemical evolution compared with values in primitive meteorites