摘要
Recently,rapid multiwavelength photometry and flash spectra of supernova(SN)2013fs imply that the progenitor stars of regular type Ⅱ supernovae(SNe Ⅱ)may be commonly surrounded by a confined,dense stellar wind ejected from the progenitor star at a large mass loss rate over few years before the SNe.Based on the assumption that the pre-SN progenitor stars of SNe Ⅱ emit wind similar to SN 2013fs,with a mass loss rate■,we investigated neutrino emissions during the wind breakouts of SN shocks.We find that a typical SNe Ⅱ can convert～10^(-3)of their bulk kinetic energy into neutrino emissions,contributing a significant fraction of the IceCube-detected neutrino flux at ■300 TeV.Moreover,■200 TeV IceCube neutrinos can be accounted for by the cosmic rays produced by shocks of all SN remnants,losing energy in their host galaxies,i.e.,the starburst galaxies.The future follow-up observations of high energy neutrinos and gamma-rays from nearby individual SNe Ⅱ,days to weeks after the explosions,will test this model.
Recently,rapid multiwavelength photometry and flash spectra of supernova(SN)2013fs imply that the progenitor stars of regular type Ⅱ supernovae(SNe Ⅱ)may be commonly surrounded by a confined,dense stellar wind ejected from the progenitor star at a large mass loss rate over few years before the SNe.Based on the assumption that the pre-SN progenitor stars of SNe Ⅱ emit wind similar to SN 2013fs,with a mass loss rate■,we investigated neutrino emissions during the wind breakouts of SN shocks.We find that a typical SNe Ⅱ can convert～10^(-3)of their bulk kinetic energy into neutrino emissions,contributing a significant fraction of the IceCube-detected neutrino flux at ■300 TeV.Moreover,■200 TeV IceCube neutrinos can be accounted for by the cosmic rays produced by shocks of all SN remnants,losing energy in their host galaxies,i.e.,the starburst galaxies.The future follow-up observations of high energy neutrinos and gamma-rays from nearby individual SNe Ⅱ,days to weeks after the explosions,will test this model.
基金
supported by the National Natural Science Foundation of China(Grant No.11773003)
the National Basic Research Program of China(973 Program)(Grant No.2014CB845800)
