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