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Rapidly rotating and strongly magnetized protoneutron stars (PNSs) created incore-collapse supernovae can drive relativistic magnetized winds. Ions andneutrons can be co-accelerated while they remain coupled through elasticcollisions. We investigate the nucleosynthesis and subsequent nucleardisintegration, and find that relativistic neutrons can be generated in suchmagnetized winds. Upon eventual decoupling, resulting inelastic collisions withejecta lead to pion production, resulting in $0.1-10\,{\rm GeV}$ neutrinos.Following this scenario presented in Murase, Dasgupta & Thompson, Phys. Rev. D,89, 043012 (2014), we numerically calculate the spectra and light curves ofquasithermal neutrino emission and find that power-law tails are formed withoutcosmic-ray acceleration. In the event of a Galactic supernova, $\sim 10-1000$neutrino events could be detected with Hyper-Kamiokande, KM3Net-ORCA andIceCube-Upgrade for PNSs with surface magnetic field $B_{\rm dip}\sim10^{13-15}\,{\rm G}$ and initial spin period $P_i \sim 1-30\,{\rm ms}$.Successful detection will enable us to study supernovae as multienergy neutrinosources and may provide clues to the roles of PNSs in diverse classes oftransients.

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