Production of the p-process nuclei in SNe Ia

The seed abundances are obtained by calculating the s-process nucleosynthesis that is expected to occur in the repeating helium shell flashes on the carbon-oxygen (CO) white dwarf (WD) during mass accretion from a binary companion. When the deflagration wave passes through the outer layer of the CO WD, p-nuclei are produced by photodisintegration reactions on s-nuclei in a region where the peak temperature ranges from 1.9 to 3.6x10^9^K. We confirm the sensitivity of the p-process on the initial distribution of s-nuclei.

We show that the initial C/O ratio in the WD does not affect much the yield of p-nuclei. On the other hand, the abundance of ^22^Ne left after s-processing has a large influence on the p-process via the ^22^Ne({alpha},n) reaction. We find that about 50% of p-nuclides are co-produced when normalized to their solar abundances in all adopted cases of seed distribution.