Gamma-ray spectra and energy deposition for type IA supernovae

Details Gamma-ray spectra and energy deposition for type IA supernovae Gamma-ray spectra and energy deposition for type IA supernovae

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...325..820a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 325, Feb. 15, 1988, p. 820-827. NSERC-supported research.

Statistics

Computation

44

Computational Astrophysics, Energy Absorption, Gamma Ray Astronomy, Gamma Ray Spectra, Supernovae, Compton Effect, Gamma Ray Absorption, Luminosity, Monte Carlo Method, Stellar Models, White Dwarf Stars

Scientific paper

The standard model for supernovae of Type Ia (SNIa) involves the synthesis of radioactive 56Ni, and it is the energy deposited by the γ-rays released in the subsequent decays that is believed to power the light curve. The authors present the results of Monte Carlo calculations of the γ-ray spectra for a grid of models that spans the parameter space associated with the radioactive decay model of SNIa. They give tables of equivalent widths and background flux levels for three of the strongest lines in the γ-ray spectrum, at 0.511, 0.847, and 1.238 MeV. Also given is a table of net γ-ray and X-ray luminosities.

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