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We calculate Galactic Chemical Evolution (GCE) of Mo and Ru by taking intoaccount the contribution from $\nu p$-process nucleosynthesis. We estimateyields 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 uponrecent models. In particular, the $\nu p$-process in energetic hypernovaeproduces a large amount of $p$-nuclei compared to the yield in ordinarycore-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 bythe $\nu p$-process. We find that the $\nu p$-process in hypernovae is the maincontributor to the elemental abundance of $^{92}$Mo at low metallicity[Fe/H$]<-2$. Our theoretical prediction of the elemental abundances inmetal-poor stars becomes more consistent with observational data when the $\nup$-process in hypernovae is taken into account.

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