[Submitted on 1 Jun 2023]
Neutrino-induced reactions on 18O and implications of 18O mixture in water Cherenkov detectors on supernova neutrino events
Toshio Suzuki🇯🇵 · Ken'ichiro Nakazato🇯🇵 · Makoto Sakuda🇯🇵
Neutrino-nucleus reaction cross sections on 18O are evaluated by shell-model calculations and compared with those on 16O. Important contributions from Gamow-Teller transitions are noticed for 18O (\nu_e, e^{-})18F in contrary to the case for 16O, where spin-dipole transitions are dominant contributions. Calculated cross sections for 18O(\nu_e, e^{-})18F are shown to be larger than for 16O at low neutrino energies below 20 MeV in natural water with the 0.205% admixture of 18O due to the lower threshold energy (1.66 MeV) for 18O than that for 16O (15.42 MeV). The resulting electron spectra, that is, the cross sections as functions of emitted electron energy Te, are also shown to be quite different, reflecting the different threshold energies. The electron spectra from (\nu_e, e^{-}) reactions on 18O and 16O in water Cherenkov detectors for supernova neutrino detection are investigated for both the cases with and without the neutrino oscillation and compared with those of the neutrino-electron scattering. It has been shown that the contribution from 18O (0.205% mixture) enhances the rates from 16O by 60% for the case without the oscillation and by 20-30% for the case with the oscillation below Te =20 MeV. For the case with the neutrino oscillation, the event rates for 18O and 16O become comparable to those of the neutrino-electron scattering. However, their rates at low energy (Te < 20 MeV) are much smaller than those of the neutrino-electron scattering, which is important for the pointing accuracy to the supernova direction.
- Comments:
- 22 pages, 7 figures
- Subjects:
- Nuclear Theory (nucl-th); Solar and Stellar Astrophysics (astro-ph.SR)
- arXiv:
- 2306.00277 [pdf]