Abstract
We calculate the Galactic Chemical Evolution of Mo and Ru by taking into account the contribution from ν
p-process nucleosynthesis. We estimate yields of p-nuclei such as 92,94Mo and 96,98Ru through the ν
p-process in various supernova progenitors based upon recent models. In particular, the ν
p-process in energetic hypernovae produces a large amount of p-nuclei compared to the yield in ordinary core-collapse SNe. Because of this, the abundances of 92,94Mo and 96,98Ru in the Galaxy are significantly enhanced at [Fe/H] = 0 by the ν
p-process. We find that the ν
p-process in hypernovae is the main contributor to the elemental abundance of 92Mo at low metallicity [Fe/H] < −2. Our theoretical prediction of the elemental abundances in metal-poor stars becomes more consistent with observational data when the ν
p-process in hypernovae is taken into account.
Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution
