Possible effects of collective neutrino oscillations in the three flavor multi-angle simulations on supernova $\nu p$ process

Abstract

We study the effects of collective neutrino oscillations on $\nu p$ process nucleosynthesis in proton-rich neutrino-driven winds by including both the multi-angle $3\times 3$ flavor mixing and the nucleosynthesis network calculation. The number flux of energetic electron antineutrinos is raised by collective neutrino oscillations in a $1$D supernova model for $40M_{\odot }$ progenitor. When the gas temperature decreases down to $\sim 2-3\times 10^9$ K, the increased flux of electron antineutrinos promotes $\nu p$ process more actively, resulting in the enhancement of $p$-nuclei. In the early phase of neutrino-driven wind, blowing at $0.6$ s after core bounce, oscillation effects are prominent in inverted mass hierarchy and $p$-nuclei are synthesized up to ${}^{106}\mathrm{Cd}$ and ${}^{108}\mathrm{Cd}$. On the other hand, in the later wind trajectory at $1.1$ s after core bounce, abundances of $p$-nuclei are increased remarkably by $\sim 10-10^4$ times in normal mass hierarchy and even reaching heavier $p$-nuclei such as ${}^{124}\mathrm{Xe}$, ${}^{126}\mathrm{Xe}$ and ${}^{130}\mathrm{Ba}$. The averaged overproduction factor of $p$-nuclei is dominated by the later wind trajectories. Our results demonstrate that collective neutrino oscillations can strongly influence $\nu p$ process, which indicates that they should be included in the network calculations in order to obtain precise abundances of $p$-nuclei. The conclusions of this paper depend on the difference of initial neutrino parameters between electron and non-electron antineutrino flavors which is large in our case. Further systematic studies on input neutrino physics and wind trajectories are necessary to draw a robust conclusion. However, this finding would help understand the origin of solar-system isotopic abundances of $p$-nuclei such as ${}^{92,94}\mathrm{Mo}$ and ${}^{96,98}\mathrm{Ru}$.

arXiv comment15 pages, 8 figures, accepted for publication in Phys.Rev.D

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