Neutrino emission from nearby supernova progenitors

14th International Conference on Topics in Astroparticle and Underground Physics

物理学;天文学

Yoshida, Takashi^1,2 ; Takahashi, Koh^1 ; Umeda, Hideyuki^1

Department of Astronomy, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo

113-0033, Japan^1

Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo-ku, Kyoto

606-8502, Japan^2

关键词: Electron-positron pairs;    Energy spectra;    Liquid Scintillation;    Mass hierarchy;    Neutrino detectors;    Neutrino emission;    Supernova explosion;    Supernova neutrinos;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/718/6/062073/pdf
DOI  :  10.1088/1742-6596/718/6/062073

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

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 Moduring the Si burning and core-collapse stages. The neutrino emission rate increases from ∼ 1050s-1to ∼ 1052s-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 veevents in the normal and inverted mass hierarchies, respectively, if a supernova explosion of a 12-20 Mostar 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.