Collective Neutrino Flavor Oscillations And Supernova Nucleosynthesis In Proton-rich Gas Flows

In core-collapse supernovae, non-linear effects are caused by self-interacting neutrinos emitted from the proto-neutron star. These many-body effects induce collective neutrino oscillations and dramatic flavor changes in neutrino fluxes which will have crucial effects on $\nu$-process in outer layers or explosive nucleosynthesis such as $r$-process and $\nu p$-process in neutrino-driven winds. We have studied collective neutrino oscillations in the realistic 3 flavor multi-angle calculation using the simulation data of 1D explosion model. We have also applied these oscillation results to the nucleosynthesis in a proton-rich gas trajectory consistently. Especially, in normal neutrino mass hierarchy, we find the enhancement of the $\bar{\nu}_{e}$ flux caused by collective neutrino oscillations before $\nu p$-process proceeds actively. Therefore, $\nu p$-process is triggered by more free neutrons produced by the $\bar{\nu}_{e}$ absorption on protons and this nucleosynthesis is successful to raise up the abundances of lighter $p$-nucleus such as Se, Kr, and Sr greatly. Heavier $p$-nucleus like $^{92}\mathrm{Mo}$ and $^{96}\mathrm{Ru}$ are expected to enhanced by collective neutrino oscillations in more proton-rich and slower gas flows.