Expectation for the MeV Gamma-Ray Emission from Pair-Instability Supernovae

Abstract

Pair-instability supernovae (PISNe) are predicted thermonuclear explosions of massive stars with helium core masses exceeding $\sim 65M_{\odot }$ and synthesize substantial amounts of radioactive ${}^{56}\mathrm{Ni}$ ($M({}^{56}\mathrm{Ni})\sim 60M_{\odot }$ in extreme cases). To investigate their observational signatures, we developed a multi-D Monte Carlo radiation transport code, assuming spherical symmetry in the background medium and the photon sources distribution, and performed simulations of gamma-ray and hard X-ray emissions from the decay chain ${}^{56}\mathrm{Ni}\to {}^{56}\mathrm{Co}\to {}^{56}\mathrm{Fe}$. We find that key gamma-ray lines (847 and 1238 keV) from ${}^{56}\mathrm{Co}$ decay in the $130M_{\odot }$ helium core model can be detected up to 300-400 Mpc by next-generation MeV gamma-ray telescopes. In contrast, the signals from the $100M_{\odot }$ model remain below the detection limits. Our results provide the template for gamma-ray follow-up observations of PISNe. Considering theoretical predictions and observational constraints, we estimate PISN event rates within 300 Mpc to be approximately 0.01-0.1 events per year, highlighting their rarity but also emphasizing their feasibility as targets for future gamma-ray observations over the decade.

arXiv comment11 pages, 6 figures, accepted for publication in The Astrophysical Journal

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