  We explore SNIa as p-process sources in the framework of two-dimensional SNIa
models using enhanced s-seed distributions as directly obtained from a sequence
of thermal pulse instabilities. The SNIa WD precursor is assumed to have
reached the Chandrasekhar mass limit in a binary system by mass accretion from
a giant/main sequence companion. We apply the tracer-particle method to
reconstruct the nucleosynthesis from the thermal histories of Lagrangian
particles, passively advected in the hydrodynamic calculations. For each
particle we follow the explosive nucleosynthesis with a detailed nuclear
reaction network. We select tracers within the typical temperature range for
p-process production, 1.5-3.7 109K, and analyse in detail their behaviour,
exploring the influence of different s-process distributions on the p-process
nucleosynthesis. We find that SNIa contribute to a large fraction of p-nuclei,
both the light p-nuclei and the heavy-p nuclei at a quite flat average
production factor. For the first time, the very abundant Ru and Mo p-isotopes
are reproduced at the same level as the heavy p-nuclei. We investigate the
metallicity effect on the p-process production. Starting with a range of
s-seeds distributions obtained for different metallicities, running SNIa
two-dimensional models and using a simple chemical evolution code, we give
estimates of the SNIa contribution to the solar p-process composition. We find
that SNIa contribute for at least 50% at the solar p-nuclei composition, in a
primary way.
