Supernova neutrinos are weakly interactive elementary particles produced during a core-collapse supernova explosion.[1] A massive star collapses at the end of its life, emitting on the order of 1058 neutrinos and antineutrinos in all lepton flavors.[2] The luminosity of different neutrino and antineutrino species are roughly the same.[3] They carry away about 99% of the gravitational energy of the dying star as a burst lasting tens of seconds.[4][5] The typical supernova neutrino energies are 10 to 20 MeV.[6] Supernovae[a] are considered the strongest and most frequent source of cosmic neutrinos in the MeV energy range.
Since neutrinos are generated in the core of a supernova, they play a crucial role in the star's collapse and explosion.[7] Neutrino heating is believed to be a critical factor in supernova explosions.[1] Therefore, observation of neutrinos from supernovae provides detailed information about core collapse and the explosion mechanism.[8] Further, neutrinos undergoing collective flavor conversions in a supernova's dense interior offers opportunities to study neutrino-neutrino interactions.[9] The only supernova neutrino event detected so far is SN 1987A.[b] Nevertheless, with current detector sensitivities, it is expected that thousands of neutrino events from a galactic core-collapse supernova would be observed.[11] The next generation of experiments are designed to be sensitive to neutrinos from supernova explosions as far as Andromeda or beyond.[12] The observation of supernovae will broaden our understanding of various astrophysical and particle physics phenomena.[13] Further, coincident detection of supernova neutrino in different experiments would provide an early alarm to astronomers about a supernova.[14]
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