  The bulk of p isotopes is created in the 'gamma processes' mainly by
sequences of photodisintegrations 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. (2011, TRV11) 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. Here we present a detailed study of
p-process nucleosynthesis occuring in SNIa with s-process seeds at different
metallicities. Based on the delayed-detonation model DDT-a of TRV11, we analyze
the dependence of p-nucleosynthesis on the s-seed distribution obtained from
different strengths of the 13C-pocket. Using a Galactic chemical evolution code
(see Travaglio et al. 2004) we study the contribution of SNIa to the solar
stable p-nuclei. We find that explosions of Chandrasekhar-mass single
degenerate systems produce a large amount of p-nuclei in our Galaxy, both in
the range of light (A < 120) and heavy p-nuclei, at almost flat average
production factors (within a factor of about 3). We discussed in details
p-isotopes such as 94Mo with a behavior diverging from the average, which we
attribute to uncertainties in the nuclear data or in SNIa modelling.
