K. Maeda, Y. Terada, D. Kasen, F. K. Roepke, A. Bamba, R. Diehl, K. Nomoto, M. Kromer, I. R. Seitenzahl, H. Yamaguchi, T. Tamagawa, W. Hillebrandt
We perform multi-dimensional, time-dependent radiation transfer simulations for hard X-ray and $\gamma$-ray emissions, following radioactive decays of $^{56}$Ni and $^{56}$Co, for two-dimensional delayed detonation models of Type Ia supernovae (SNe Ia). The synthetic spectra and light curves are compared with the sensitivities of current and future observatories with an exposure of $10^6$ seconds. The non-detection of the $\gamma$-ray signal from SN 2011fe at 6.4 Mpc by SPI on board INTEGRAL places the upper limit for the mass of $^{56}$Ni as $\lsim$$1.0 M_{\odot}$ independently from observations in any other wavelengths. Signals from the newly formed radioactive species have not been convincingly measured yet from any SN Ia, but the future X-ray and $\gamma$-ray missions are expected to deepen the observable horizon to provide the high energy emission data for a significant SN Ia sample. We predict that the hard X-ray detectors on board NuStar or ASTRO-H, launched in 2012 and to be so in 2014, will reach to SNe Ia at $\sim$15 Mpc, i.e., one SN in a few years. Furthermore, according to the present results, the soft $\gamma$-ray detector on board ASTRO-H will be able to detect the 158 keV line emission up to $\sim$25 Mpc, i.e., a few SNe Ia per year. Proposed next generation $\gamma$-ray missions, e.g., GRIPS, could reach to SNe Ia at $\sim$$20 - 35$ Mpc by MeV observations. Those would provide new diagnostics and strong constraints on explosion models, detecting rather directly the main energy source of supernova light.
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http://arxiv.org/abs/1208.2094
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