Gamma-Rays from Heavy Nuclei Accelerated in Supernova Remnants

TL;DR

This paper explores how supernova remnants accelerate protons and heavy nuclei, influencing cosmic ray spectra and gamma-ray emissions through a semi-analytical model that considers magnetic fields, shock dynamics, and nuclear interactions.

Contribution

It introduces a self-consistent semi-analytical framework for modeling particle acceleration and gamma-ray emission in supernova remnants, emphasizing the role of heavy nuclei.

Findings

Heavy nuclei are significant in shock dynamics and gamma-ray production.

The model links cosmic ray spectra with supernova remnant properties.

Nuclear interactions produce observable gamma-ray signatures.

Abstract

We investigate the theoretical and observational implications of the acceleration of protons and heavier nuclei in supernova remnants (SNRs). By adopting a semi-analytical technique, we study the non-linear interplay among particle acceleration, magnetic field generation and shock dynamics, outlining a self-consistent scenario for the origin of the spectrum of Galactic cosmic rays as produced in this class of sources. Moreover, the inferred chemical abundances suggest nuclei heavier than Hydrogen to be relevant not only in the shock dynamics but also in the calculation of the gamma-ray emission from SNRs due to the decay of neutral pions produced in nuclear interactions.