Quasithermal GeV neutrinos from neutron-loaded magnetized outflows in core-collapse supernovae: Spectra and light curves

Rapidly rotating and strongly magnetized protoneutron stars (PNSs) created in core-collapse supernovae can drive relativistic magnetized winds. Ions and neutrons can be coaccelerated while they remain coupled through elastic collisions. We investigate the nucleosynthesis and subsequent nuclear disintegration, and find that relativistic neutrons can be generated in such magnetized winds. Upon eventual decoupling, resulting inelastic collisions with ejecta lead to pion production, resulting in 0.1--10 GeV neutrinos. Following this scenario presented in Murase et al. [Quasithermal neutrinos from rotating protoneutron stars born during core collapse of massive stars, Phys. Rev. D, 89, 043012 (2014)], we numerically calculate the spectra and light curves of quasithermal neutrino emission. In the event of a Galactic supernova, $\ensuremath{\sim}10--1000$ neutrino events could be detected with Hyper-Kamiokande, KM3Net-ORCA, and IceCube-Upgrade for PNSs with surface magnetic field ${B}_{\mathrm{dip}}\ensuremath{\sim}{10}^{13--15}\text{ }\text{ }\mathrm{G}$ and initial spin period ${P}_{i}\ensuremath{\sim}1--30\text{ }\text{ }\mathrm{ms}$. Successful detection will enable us to study supernovae as multienergy neutrino sources and may provide clues to the roles of PNSs in diverse classes of transients.