Understanding hadronic gamma-ray emission from supernova remnants

TL;DR

This paper investigates whether gamma-ray emissions from supernova remnants are of hadronic origin, considering magnetic field amplification effects and pre-supernova winds, to align theoretical models with observational data.

Contribution

It introduces a phenomenological model incorporating magnetic field amplification and pre-supernova wind effects to explain gamma-ray emissions from supernova remnants.

Findings

Magnetic field amplification influences particle spectra significantly.

Pre-supernova winds affect the gamma-ray luminosity evolution.

The proposed scenario aligns with current gamma-ray observational data.

Abstract

We aim to test the plausibility of a theoretical framework in which the gamma-ray emission detected from supernova remnants may be of hadronic origin, i.e., due to the decay of neutral pions produced in nuclear collisions involving relativistic nuclei. In particular, we investigate the effects induced by magnetic field amplification on the expected particle spectra, outlining a phenomenological scenario consistent with both the underlying Physics and the larger and larger amount of observational data provided by the present generation of gamma experiments, which seem to indicate rather steep spectra for the accelerated particles. In addition, in order to study to study how pre-supernova winds might affect the expected emission in this class of sources, the time-dependent gamma-ray luminosity of a remnant with a massive progenitor is worked out. Solid points and limitations of the proposed scenario are finally discussed in a critical way.