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

## TL;DR

This paper discusses how gamma-ray observations of Type Ia supernovae, specifically SN2014J, reveal details about their explosion physics and structure, highlighting the presence of high-velocity nickel plumes.

## Contribution

It provides new insights into the explosion mechanism of SNIa through gamma-ray data, especially the detection of nickel in outer layers, which challenges existing models.

## Key findings

- Detection of gamma-ray lines from SN2014J supports high-velocity nickel plumes.
- Gamma-ray data suggests a different explosion geometry than traditional models.
- Implications for understanding the progenitor systems of 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 $^{56}$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.