Abstract
Recent progress of neutrino detectors makes it possible to detect pre-SN neutrinos, which are emitted from the core of massive stars before supernova explosions. Pre-SN neutrino observations will become an alarm for supernovae. We hence calculate the number luminosity and energy spectra of pre-SN neutrinos from the 15 M ⊙ progenitor based on the state-of-the-art calculations of massive stars. We find that the number luminosity of ve ’s is before core collapse and core bounce, respectively, whereas that of ’s becomes largest around core collapse . We then estimate the number of neutrino events at neutrino detectors taking neutrino oscillations into the obtained luminosities and spectra. We find that an alarm is issued a few days before the explosion by detecting ’s at liquid-scintilation type detectors if the progenitor is located at 200 pc. Finally, we perform a systematic study of pre-SN neutrino emission for 7 progenitor models with different initial masses. We find that the difference of the number luminosities is ~ 1 order and the dependence of the initial mass have to be taken into the theoretical predictions of pre-SN neutrino observations.
Highlights
Neutrino astronomy has begun at the historical supernova event SN1987A
Recent progress of neutrino detectors makes it possible to detect pre-SN neutrinos, which are emitted from the core of massive stars before supernova explosions
Pre-SN neutrinos may be observed firstly in the evolution of massive stars located at our vicinity and their detection will make us possible to surely observe the subsequent supernova explosions, which is referred to occur once per centry
Summary
Neutrino detectors at that time detected 24 neutrinos for the first time [1] and we obtained the luminosity and average energy of supernova neutrinos Lν ∼ 5 × 1052 ergs, Eν ∼ 10-12 MeV [2] They are consistent with theoretical predictions based on the neutrino heating mechanism, which is one of the favored mechanisms of core-collapse supernovae, and our understanding of supernova explosion has been developed greatly. A shock wave is formed between the accretion and stable parts (core bounce) and propagates outward If it reaches the stellar surface, the supernova explosion occurs. Pre-SN neutrinos may be observed firstly in the evolution of massive stars located at our vicinity and their detection will make us possible to surely observe the subsequent supernova explosions, which is referred to occur once per centry. It is strongly required to establish an alert system with pre-SN neutrinos
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