Gamma-rays from SNIa

Abstract : 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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Communication dans un congrès
Frontier Research in Astrophysics - II, May 2016, Mondello, Italy. PoS, FRAPWS2016, pp.035, 2017, 〈10.22323/1.269.0035〉
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https://hal.archives-ouvertes.fr/hal-01669723
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Soumis le : jeudi 21 décembre 2017 - 00:14:37
Dernière modification le : mercredi 12 décembre 2018 - 08:44:30

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J. Isern, E. Bravo, P. Jean. Gamma-rays from SNIa. Frontier Research in Astrophysics - II, May 2016, Mondello, Italy. PoS, FRAPWS2016, pp.035, 2017, 〈10.22323/1.269.0035〉. 〈hal-01669723〉

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