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 40 M _ { \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 } .