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We study the nucleosyntheses of the light elements 7Li and 11B and ther-process elements in Type II supernovae from the point of view of supernovaneutrinos and Galactic chemical evolution. We investigate the influence of theluminosity and average energy (temperature) of supernova neutrinos on these twonucleosynthesis processes. Common models of the total energy E_nu and the decaytime of the neutrino luminosity tau_nu of supernova neutrinos are adopted tounderstand both processes. We adopt the model of the supernova explosion of a16.2 M_odot star, which corresponds to SN 1987A, and calculate thenucleosynthesis of the light elements by the postprocessing. We find that theejected masses of 7Li and 11B are roughly proportional to the total neutrinoenergy and weakly dependent on the decay time of the neutrino luminosity. Asfor the r-process nucleosynthesis, we adopt the same models of the neutrinoluminosity in the neutrino-driven wind models of a 1.4 M_odot neutron star. Wefind that the r-process nucleosynthesis is affected through the peak neutrinoluminosity, which depends on E_nu/tau_nu. We also discuss the unresolvedproblem of the overproduction of 11B in the Galactic chemical evolution of thelight elements. We have to assume E_{nu} < 1.2 \times 10^{53} ergs to avoid theoverproduction of 11B, which is too small to accept in comparison to 3.0 \times10^{53} ergs deduced from the observation of SN1987A. We propose to reduce thetemperature of nu_{mu, tau} and their anti-particles to T_{nu_{mu, tau}} =T_{bar{nu}_{mu,tau}} = 6.0 MeV/k. This modification of the neutrino temperatureis shown to resolve the overproduction problem of 11B while still keeping asuccessful r-process abundance pattern.Comment: 29 pages, 5 figures, Astrophys. J., in pres

Nucleosynthesis of Light Elements and Heavyr‐Process Elements through the ν‐Process in Supernova Explosions