Merger and non-merger galaxy clusters in cosmological AMR simulations

TL;DR

This paper uses high-resolution cosmological simulations to study how shocks, cosmic ray acceleration, and turbulence vary with the dynamical state of galaxy clusters, revealing significant differences among post-merger, merging, and relaxed systems.

Contribution

It introduces a detailed simulation approach to analyze the impact of cluster dynamical states on non-thermal phenomena in galaxy clusters.

Findings

Differences in shock properties among cluster states

Variation in cosmic ray acceleration efficiency

Turbulence levels depend on cluster dynamical status

Abstract

Aims: We discuss the dependence of shocks, cosmic rays acceleration and turbulence on the dynamical state of the host clusters. Method: We perform cosmological simulations with the grid code ENZO 1.5, with a mesh refinement scheme tailored to follow at high resolution shocks and turbulence developed in the clusters volume. Results: Sizable differences are found when some important properties, connected to non-thermal activity in clusters, are compared for post-merger, merging and relaxing systems.