# Gamma rays from reaccelerated particles at supernova remnant shocks

## TL;DR

This paper explores how gamma-ray observations of supernova remnants can shed light on the reacceleration of particles at shock fronts, influenced by magnetic field orientation, with implications for cosmic ray physics.

## Contribution

It introduces the role of shock obliquity and reacceleration in supernova remnants, linking gamma-ray data to particle acceleration mechanisms and cosmic ray spectra.

## Key findings

- Gamma-ray observations can diagnose reacceleration processes.
- Shock obliquity affects particle injection and acceleration.
- Reacceleration impacts secondary cosmic ray nuclei spectra.

## Abstract

Diffusive shock acceleration is considered as the main mechanism for particle energization in supernova remnants, as well as in other classes of sources. The existence of some remnants that show a bilateral morphology in the X-rays and gamma rays suggests that this process occurs with an efficiency that depends upon the inclination angle between the shock normal and the large scale magnetic field in which the shock propagates. This interpretation is additionally supported by recent particle-in-cell simulations that show how ions are not injected if the shock is more oblique than $\sim 45^{o}$. These shocks provide an excellent test bench for the process of reacceleration at the same shock: non-thermal seed particles that are reached by the shock front are automatically injected and accelerated. This process was recently discussed as a possible reason for some anomalous behaviour of the spectra of secondary cosmic ray nuclei. Here we discuss how gamma--ray observations of selected supernova remnants can provide us with precious information about this process and lead us to a better assessment of particle diffusive shock reacceleration for other observables in cosmic ray physics.