The interplay between cosmic rays and magnetic turbulence in galaxy clusters: radio halos and gamma rays

TL;DR

This paper explores how magnetic turbulence influences cosmic ray behavior and non-thermal emissions like radio halos and gamma rays in galaxy clusters, highlighting recent modeling advances.

Contribution

It provides a comprehensive review of turbulence physics and introduces new models linking turbulence to observed non-thermal emissions in galaxy clusters.

Findings

Turbulence impacts cosmic ray acceleration in galaxy clusters.

Models successfully reproduce observed radio halos.

Turbulent processes are key to understanding gamma-ray emissions.

Abstract

The interaction of magnetic turbulence and relativistic particles is a important process for understanding particles propagation and acceleration in many astrophysical environments. Large-scale turbulence can be generated in the intra-cluster-medium (ICM) during mergers between galaxy clusters and affects their non-thermal properties. Giant radio halos, Mpc-scale synchrotron sources observed in merging clusters, may probe the connection between turbulence and non-thermal cluster-scale emission. After discussing relevant aspects of the physics of turbulence and turbulent acceleration in the ICM, I will focus on recent advances in the modeling of non-thermal emission from galaxy clusters.