Energy Spectrum of Ultra High Energy γ-Rays from Supernova

概要

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If a newly born neutron star in SN1987A is a powerful injector of ultra high energy (UHE) protons, UHE γ-rays will be emitted by bombardment of supernova ejecta with these UHE particles. We compute energy spectrum of the UHE γ-rays generated by monoenergetic protons using Monte-Carlo simulations at the period of high flux when the column density is 30〜100g/cm^2. If the column density of the ejecta is less than 〜100g/cm^2, low energy γ-rays do not increase as E^<-2>, like the case for Cyg X-3, but they have much harder spectrum close to E^<-1>. The expected numbers of PeV and TeV region γ-rays per hour are at least 0.16 counts (L_p/10^<41> ergs)(S/(50m)^2)(d/56kpc)^<-2> and 132 counts (L_p/10^<41> ergs)(S/30000m^2)(d/56kpc)^<-2> where L_p, S and d are the proton luminosity, the area of detectors, and the distance to LMC, respectively.
理論物理学刊行会の論文
1988-02-25