The p-Process Nucleosynthesis in the Carbon Deflagration Model for Type Ia Supernovae Original Research Article

We calculate nucleosynthesis of proton-rich isotopes in the Carbon deflagration model for Type Ia supernovae (SNe Ia). We investigate the influence of variations in the C/O ratios and 22Ne abundance left in accreting CO white dwarf on the p-process nucleosynthesis and the sensitivity of the seed abundance distribution. We find that about 55% of the p-nuclides are produced at the levels that can explain the solar abundances in all adopted cases of initial compositions. Mo and Ru isotopes severely deficient in Type II supernovae (SNe II) are enhanced by a factor of ∼10, but unavoidable underproduction still exists. We also compare the yields of 56Fe and p-nuclei in SNe Ia and SNe II, and obtain a result that C-deflagration supernovae can contribute to the galactic evolution (and the solar system) of the p-nuclei if the s-process occurs in accreting CO white dwarfs at the similar efficiency as in AGB stars.