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24 April 2024 |
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Prospect of Studying Hard X- and Gamma-Rays from Type Ia Supernovae | | 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
; | | Date: |
10 Aug 2012 | | Abstract: | 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. | | Source: | arXiv, 1208.2094 | | Services: | Forum | Review | PDF | Favorites | |
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