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Production of the $$p$$-process nuclei in the carbon-deflagration model for type Ia supernovae

Kusakabe, Motohiko*; Iwamoto, Nobuyuki  ; Nomoto, Kenichi*

We calculate nucleosynthesis of proton-rich isotopes in the carbon deflagration model for Type Ia supernovae (SNe Ia). When the deflagration wave passes through the outer layer of the CO white dwarf, $$p$$-nuclei are produced by photodisintegration reactions on s-nuclei in a region with the peak temperature ranging from 1.9 to 3.6$$times$$10$$^{9}$$ K. We find that about 50% of $$p$$-nuclides are co-produced when normalized to their solar abundances in all adopted cases of seed distribution. Mo and Ru, which are largely underproduced in Type II supernovae (SNe II), are produced at a level similar to other $$p$$-nuclides. The ratios between $$p$$-nuclei and iron in the ejecta are larger than the solar ratios by a factor of 1.2. We also compare the yields of oxygen, iron, and $$p$$-nuclides in SNe Ia and SNe II, and suggest that SNe Ia could make a larger contribution than SNe II to the solar system content of $$p$$-nuclei.

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