6th Symposium on Neutrinos and Dark Matter in Nuclear Physics 2018

Neutrino-nucleus reactions and e-capture rates based on new shell-model Hamiltonians

Not scheduled

30m

IBS HQ, Daejeon, Korea

Oral

Speakers

Prof. Baha Balantekin (University of Wisconsin)Prof. Toshio Suzuki (Nihon University)Prof. Toshitaka Kajino (National Astronomical Observatory of Japan)

Description

Neutrino-nucleus reaction cross sections relevant to supernova neutrino detection and nucleosynthesis are evaluated for ${}^{12}$C, ${}^{13}$C, ${}^{16}$O, ${}^{40}$Ar and ${}^{56}$Ni with new shell-model Hamiltonians. Cross sections for various gamma and particle emission channels as well as for coherent scattering are obtained for ${}^{12}$C, ${}^{13}$C and ${}^{16}$O. The updated cross sections are compared with available experimental data as well as previous calculations. Advantage of using light targets for coherent scattering is discussed. Charged-current cross sections folded over neutrino spectra with and without the neutrino oscillations are compared to each other to see how they are sensitive to the MSW and/or collective neutrino oscillation effects. We also discuss electron-capture rates for supernova explosions and evolution of stars updated with new shell-model Hamiltonians for $sd$- and $pf$-shells. Evaluations of the rates for two-major shells such as $sd$-$pf$ and $pf$-$g$ shells are also in progress.