BEXCO - Room F(201/202/203/204)
[CRI154] High-Energy Cosmic-Rays and Neutrinos around Supernova Shock Breakout
Supernovae occurring in dense winds are promising candidates for particle acceleration to high energies. We focus here on the onset of particle acceleration, during the first couple of days following core-collapse. We show that a collisionless shock rapidly forms at supernova shock breakout. We calculate, for the first time, the maximum CR energy that can be reached with Bell's non-resonant hybrid instability in such environments. We take the effect of cosmic-ray energy losses due to inelastic p p and p gamma collisions into account, as well as possible damping of the turbulence by radiation. We find that protons are rapidly accelerated to multi-TeV energies (within a few minutes for a Wolf-Rayet progenitor, and a few hours for a red supergiant). Secondary high-energy neutrinos with energies greater than ~ 100 GeV are expected to be produced. We calculate their flux, depending on the parameters of the circumstellar environment.