Characterizing the magnetic field in the intracluster medium

TL;DR

This paper investigates magnetic field turbulence in the intracluster medium using numerical simulations in MHD and KMHD frameworks, analyzing polarization maps to understand the physical processes in galaxy clusters.

Contribution

It introduces a comparative analysis of magnetic turbulence in ICM using both MHD and KMHD simulations, focusing on polarization signatures.

Findings

Magnetic field structures influence polarization maps significantly.

Turbulence characteristics differ between MHD and KMHD models.

Results aid in interpreting radio observations of galaxy clusters.

Abstract

During structure formation, energetic events and random motions of the hot gas residing inside galaxy clusters (the intracluster medium, ICM) generate turbulent motions. Radio diffuse emission probes the presence of magnetic fields and relativistic particles in the ICM, being a key ingredient for understanding the physical processes at work in clusters of galaxies. In this work, we present results from numerical simulations of magnetic field turbulence in magnetohydrodynamics (MHD) and kinetic MHD (KMHD) frameworks. We characterize magnetic field structures through the imprints left on polarization maps.