Time Variation of Ultra High Energy γ-Ray from SN1987A

概要

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If the neutron star exists in the remnant of SN1987A, there is a possibility to check the acceleration activity of the pulsar in the very early phase. As indicated by the observation of Cyg X-3, the pulsar may generate a proton beam with energy up to 10^<17>eV, which interacts with the ejected matter and produces ultra high energy (UHE) γ-rays as well as UHE neutrinos with energy up to 10^<16> eV. Luminosity of UHE γ-rays will take a maximum at 5.5 months (8.3 months) from February 23rd, if the mass ejected by the supernova explosion with energy 〜1.4×10^<17> ergs/g is 7M_⊙(15M_⊙) and if the UHE protons are not confined in the ejected by the turbulent magnetic fields. If they are completely trapped, the maximum epoch will be prolonged by the factor about 3. The proton beam luminosity will be limited to 7×10^<41>ergs/s at most if muons generated by the UHE neutrinos are not detected in the underground detectors.
理論物理学刊行会の論文
1987-11-25