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Volume 269 - Frontier Research in Astrophysics – II (FRAPWS2016) - High Energy Astrophsyics
Gamma rays from SNIa
J. Isern,* E. Bravo, P. Jean
*corresponding author
Full text: pdf
Pre-published on: 2017 August 02
Published on: 2017 November 15
Type Ia supernovae are thought to be the outcome of the thermonuclear explosion of a carbon/oxygen white dwarf in a close binary system. Their optical light curve is powered by thermalized gamma-rays produced by the radioactive decay of 56Ni, the most abundant isotope present in the debris. The maximum and the shape of the light curve strongly depends on the total amount and distribution of this freshly synthesized isotope, as well as on the velocity and density distribution of the ejecta. Gamma-rays escaping the ejecta have the advantage of their lower interaction with the ejecta, the possibility to distinguish among isotopes and the relative simplicity of their transport modelling, and can be used as a diagnostic tool for studying the structure of the exploding star and the characteristics of the explosion, as it has been proved in the case of SN2014J.
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