Impact of hypernova {\nu}p-process nucleosynthesis on the galactic chemical evolution of Mo and Ru

TL;DR

This study models how the p-process in hypernovae influences the galactic chemical evolution of molybdenum and ruthenium, showing it significantly enhances their abundances, especially at low metallicities, aligning theory with observations.

Contribution

It introduces detailed GCE modeling including p-process yields from hypernovae, highlighting their dominant role in producing Mo and Ru in the galaxy.

Findings

p-process in hypernovae produces large amounts of Mo and Ru.

Abundances of Mo and Ru are significantly enhanced at [Fe/H]=0.

Model predictions align better with observed stellar abundances when hypernova contributions are included.

Abstract

We calculate Galactic Chemical Evolution (GCE) of Mo and Ru by taking into account the contribution from $\nu p$-process nucleosynthesis. We estimate yields of $p$-nuclei such as $^{92,94}\mathrm{Mo}$ and $^{96,98}\mathrm{Ru}$ through the $\nu p$-process in various supernova (SN) progenitors based upon recent models. In particular, the $\nu p$-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 $^{92,94}\mathrm{Mo}$ and $^{96,98}\mathrm{Ru}$ in the Galaxy are significantly enhanced at [Fe/H]=0 by the $\nu p$-process. We find that the $\nu p$-process in hypernovae is the main contributor to the elemental abundance of $^{92}$Mo 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 $\nu p$-process in hypernovae is taken into account.