Abstract
Neutrinos have an important role for energy loss process during advanced evolution of massive stars. Although the luminosity and average energy of neutrinos during the Si burning are much smaller than those of supernova neutrinos, these neutrinos are expected to be detected by the liquid scintillation neutrino detector KamLAND if a supernova explosion occurs at the distance of ~100 parsec. We investigate the neutrino emission from massive stars during advanced evolution. We calculate the evolution of the energy spectra of neutrinos produced through electron-positron pair-annihilation in the supernova progenitors with the initial mass of 12, 15, and 20 M⊙ during the Si burning and core-collapse stages. The neutrino emission rate increases from ~ 1050 s-1 to ~ 1052 s-1. The average energy of electron-antineutrinos is about 1.25 MeV during the Si burning and gradually increases until the core-collapse. For one week before the supernova explosion, the KamLAND detector is expected to observe 12-24 and 6-13 v̄e events in the normal and inverted mass hierarchies, respectively, if a supernova explosion of a 12-20 M⊙ star occurs at the distance of 200 parsec, corresponding to the distance to Betelgeuse. Observations of neutrinos from SN progenitors have a possibility to constrain the core structure and the evolution just before the core collapse of massive stars.
Highlights
Supernova (SN) explosion is a final event of massive star evolution
We investigate the time evolution of the spectra of neutrinos emitted through pair neutrino process from SN progenitors during the stages from the Si burning to the corecollapse
We will show the spectra of neutrinos emitted by pair neutrino process during the core Si burning and at the last step of the calculation of the 15 M⊙ SN progenitor
Summary
Supernova (SN) explosion is a final event of massive star evolution. From C-burning, the energy generated by nuclear burning in massive stars is mainly carried out by neutrinos. The neutrino luminosity becomes ∼ 1047 erg s−1 during the Si burning This luminosity value is still much smaller than that of SN neutrinos (Lν ∼ 1053 erg s−1 ), the current neutrino detectors are expected to detect these neutrinos if a SN explosion occurs at a distance of ∼100 parsec from the earth. In order to predict the neutrino events from a SN progenitor before the SN explosion, one needs to evaluate neutrino spectra during the advanced evolution of massive stars. We investigate the time evolution of the spectra of neutrinos emitted through pair neutrino process from SN progenitors during the stages from the Si burning to the corecollapse. We evaluate the neutrino events of SN progenitors with the initial mass of 12, 15, and
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
