Cosmological simulations of the generation of cluster-scale radio emission from turbulent re-acceleration

TL;DR

This study uses cosmological simulations to explore the origin of cluster-scale radio emissions, demonstrating that turbulence-driven cosmic-ray re-acceleration can produce both classical and mega radio halos, with different turbulence properties.

Contribution

It presents the first simulation showing that turbulence-induced cosmic-ray re-acceleration can explain both classical and mega radio halos in galaxy clusters.

Findings

Simulations reproduce observed properties of radio halos during cluster mergers.

Evidence of larger-scale emission resembling mega radio halos near merger axes.

Turbulence characteristics differ between classical and mega radio halo regions.

Abstract

Context. The recent discovery of so-called mega radio halos as a new class of diffuse, steep-spectrum radio sources in clusters of galaxies has raised questions about the origin and the evolution of cluster-wide radio emission. Aims. We investigate whether the formation mechanisms of radio halos and mega radio halos differ, or whether they can be produced by different modalities of the same (re)acceleration mechanism. Here we present results of a cosmological simulation of a disturbed galaxy cluster, with the aim to study the origin of mega radio halos. Methods. We analysed the evolution of cosmic-ray electrons, subject to gains and losses using a Fokker-Planck solver. In particular, we included the effects of Adiabatic Stochastic Acceleration (ASA) which is caused by the stochastic interaction of cosmic rays with diffusing magnetic field lines in super-Alfvenic turbulence. Moreover, we included shock acceleration and the seeding of cosmic-ray electrons by galaxies. Results. Our simulations generate cluster-scale radio sources during mergers, with properties that are in agreement with those observed for real radio halos. Furthermore, we find evidence of additional emission on larger scales. This emission resembles the radial distribution and the spectrum of a mega radio halo, but only when viewed close to the merger axis. Conclusions. In our simulation, the mechanism responsible for the formation of diffuse radio emission, both in the form of classical and mega radio halos, is cosmic-ray re-acceleration by turbulence. This turbulence is more solenoidal and more subsonic in the classical radio halo region, than in the mega radio halo region.