PeV neutrinos from wind breakouts of type II supernovae

Abstract

Recently, the rapid multiwavelength photometry and flash spectra of supernova (SN) 2013fs imply that the progenitor stars of regular type II SNe (SNe II) might be commonly surrounded with a confined dense stellar wind ejected by themselves with large mass loss rate few years before the SNe. Based on the assumption that the pre-SN progenitor stars of SNe II have a SN 2013fs-like wind, with mass loss rate $\dot{M}\sim 3\times 10^{-3}(v_w/100\mathrm{km}{\mathrm{s}}^{-1}){\mathrm{M}}_{\odot }\mathrm{y}{\mathrm{r}}^{-1}$, we investigate the neutrino emission during the wind breakouts of SN shocks. We find that the regular SNe II can convert a fraction $\sim 10^{-3}$ of their bulk kinetic energy into neutrino emission, which can contribute a significant fraction of the IceCube-detected neutrino flux at $\ga300$ TeV. Moreover, the $\la200$~TeV IceCube neutrinos can be accounted for by cosmic rays produced by the shocks of all SN remnants, losing energy in their host galaxies, i.e., starburst galaxies. The future follow-up observations of neutrinos by Gen2 and gamma-rays by CTA and LHAASO from nearby individual SNe II, within weeks after the explosions, will test this model.

Accepted version; 7 pages, 2 figures. Significant changes, more extended discussion on uncertainties; max CR energy at small radii corrected; main conclusion unchanged

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