The neutrino process in core-collapse supernovaONLINE ONLY

In a core-collapse supernova, neutrinos carry a large amount of explosion energy, $10^{51-53}$ erg. Despite the small cross-section of weak interaction, such energetic neutrinos enable the elements produced by neutrino-induced reactions. Most of the elements in our solar system have been explained by $s$-, $r$-, and $p$-processes. However, still, the origin of some elements has not been explained. In particular, the elements of $^{92}$Nb, $^{98}$Tc, and $^{138}$La are rarely produced by beta decay because their neighboring nuclides in the nuclear chart are stable. The neutrino process has explained the production of those elements. And also, in this process, the neutrino interacts with the neutrino itself and the electron in the star. This leads to a change in neutrino energy distribution and affects the neutrino-induced reactions. In this talk, I would like to explain how to describe this neutrino interaction in SN environments, focusing on the Mikheyev–Smirnov–Wolfenstein effect and collective neutrino oscillation. Finally, the effects of such interactions on neutrino-process yields will be presented.