PROSPECT OF STUDYING HARD X- AND GAMMA-RAYS FROM TYPE Ia SUPERNOVAE

Journal Article · Tue Nov 20 00:00:00 EST 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/760/1/54· OSTI ID:22086312

Maeda, K; Nomoto, K ^[1]; Terada, Y ^[2]; Kasen, D ^[3]; Roepke, F K; Seitenzahl, I R ^[4]; Bamba, A ^[5]; Diehl, R ^[6]; Kromer, M; Hillebrandt, W ^[7]; Yamaguchi, H ^[8]; Tamagawa, T ^[9]

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1. Kavli Institute for the Physics and Mathematics of the Universe (Kavli-IPMU), Todai Institutes for Advanced Study (TODIAS), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583 (Japan)
2. Department of Physics, Saitama University, 255 Shimo-Okubo, Sakura-ku, Saitama 338-8570 (Japan)
3. Department of Physics, University of California at Berkeley, 366 LeConte, Berkeley, CA 94720 (United States)
4. Institut fuer Theoretische Physik und Astrophysik, Universitaet Wuerzburg, Emil-Fischer-Strasse 31, D-97074 Wuerzburg (Germany)
5. Department of Physics and Mathematics, College of Science and Engineering, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo-ku, Sagamihara, Kanagawa 252-5258 (Japan)
6. Max-Planck-Institut fuer Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching (Germany)
7. Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Strasse 1, D-85741 Garching (Germany)
8. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
9. RIKEN (Institute of Physical and Chemical Research), 2-1 Hirosawa, Wako, Saitama 351-0198 (Japan)

We perform multi-dimensional, time-dependent radiation transfer simulations for hard X-ray and {gamma}-ray emissions, following radioactive decays of {sup 56}Ni and {sup 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 for an exposure time of 10{sup 6} s. The non-detection of the {gamma}-ray signal from SN 2011fe at 6.4 Mpc by SPI on board INTEGRAL places an upper limit on the mass of {sup 56}Ni of {approx}< 1.0 M {sub Sun }, independently from observations in any other wavelengths. Signals from the newly formed radioactive species have not yet been convincingly measured from any SN Ia, but future X-ray and {gamma}-ray missions are expected to deepen the observable horizon to provide high energy emission data for a significant SN Ia sample. We predict that the hard X-ray detectors on board NuStar (launched in 2012) or ASTRO-H (scheduled for launch in 2014) will reach to SNe Ia at {approx}15 Mpc, i.e., one SN every 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 {approx}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 {approx}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.

• OSTI ID: 22086312
• Journal Information: Astrophysical Journal, Vol. 760, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ASTROPHYSICS
COBALT 56
COMPUTERIZED SIMULATION
EMISSION SPECTRA
GAMMA ASTRONOMY
GAMMA DETECTION
GAMMA RADIATION
HARD X RADIATION
KEV RANGE
MEV RANGE
NICKEL 56
NUCLEAR DECAY
NUCLEOSYNTHESIS
PHOTON EMISSION
RADIANT HEAT TRANSFER
SENSITIVITY
SUPERNOVAE
TIME DEPENDENCE
VISIBLE RADIATION
X-RAY DETECTION