Non-thermal processes in cosmological simulations

TL;DR

This paper reviews how non-thermal processes like shocks, turbulence, and magnetic fields are crucial for understanding galaxy cluster formation and their observable emissions in cosmological simulations.

Contribution

It summarizes recent simulation results on non-thermal components in galaxy clusters, highlighting their roles in cluster dynamics and emissions.

Findings

Shocks and turbulence are fundamental in cluster formation.

Magnetic fields influence heat transport and dissipation.

Cosmic rays affect observable emissions in clusters.

Abstract

Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.