Quasithermal Neutrinos from Rotating Protoneutron Stars Born during Core Collapse of Massive Stars

摘要

Rotating and magnetized protoneutron stars (PNSs) may drive relativisticmagneto-centrifugally accelerated winds as they cool immediately after corecollapse. The wind fluid near the star is composed of neutrons and protons, andthe neutrons become relativistic while collisionally coupled with the ions.Here, we argue that the neutrons in the flow eventually undergo inelasticcollisions around the termination shock inside the stellar material, producing~0.1-1 GeV neutrinos, without relying on cosmic-ray acceleration mechanisms.Even higher-energy neutrinos may be produced via particle accelerationmechanisms. We show that PINGU and Hyper-Kamiokande can detect such neutrinosfrom nearby core-collapse supernovae, by reducing the atmospheric neutrinobackground via coincident detection of MeV neutrinos or gravitational waves andoptical observations. Detection of these GeV and/or higher-energy neutrinoswould provide important clues to the physics of magnetic acceleration,nucleosynthesis, the relation between supernovae and gamma-ray bursts, and theproperties of newly born neutron stars.