Possible effects of collective neutrino oscillations in three-flavor multiangle simulations of supernova νp processes

We study the effects of collective neutrino oscillations on νp process nucleosynthesis in proton-rich neutrino-driven winds by including both the multiangle 3×3 flavor mixing and the nucleosynthesis network calculation. The number flux of energetic electron antineutrinos is raised by collective neutrino oscillations in a 1D supernova model for the 40M progenitor. When the gas temperature decreases down to ∼2-3×109 K, the increased flux of electron antineutrinos promotes the νp 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 Cd106 and Cd108. On the other hand, in the later wind trajectory at 1.1 s after core bounce, abundances of p-nuclei are increased remarkably by ∼10-104 times in normal mass hierarchy and even reaching heavier p-nuclei such as Xe124, Xe126 and Ba130. The averaged overproduction factor of p-nuclei is dominated by the later wind trajectories. Our results demonstrate that collective neutrino oscillations can strongly influence the νp 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 nonelectron 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 Mo92,94 and Ru96,98.