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