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Insights on the physics of SNIa obtained from their gamma-ray emission

J. Isern, E. Bravo, P. Jean, J. Knodlseder

in 11th INTEGRAL Conference Gamma-Ray Astrophysics in Multi-Wavelength Perspective

Contribution: pdf


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 $^{56}$Ni, the most abundant isotope present in the debris. Gamma-rays escaping the ejecta can be used as a diagnostic tool for studying the structure of the exploding star and the characteristics of the explosion. The fluxes of the $^{56}$Ni lines and the continuum obtained by INTEGRAL from
SN2014J in M82, the first ever gamma-detected SNIa, around the time of the
maximum of the optical light curve strongly suggest the presence of a plume of $^{56}$Ni in the outermost layers moving at high velocities. If this interpretation was correct, it could have important consequences on our current understanding of the physics of the explosion and on the nature of the systems that explode.