Acceleration of Cosmic Ray Electrons at Weak Shocks in Galaxy Clusters

TL;DR

This paper investigates how cosmic ray electrons are accelerated at weak shocks in galaxy clusters, explaining observed radio relics through diffusive shock acceleration and turbulence, and addressing discrepancies between X-ray and radio observations.

Contribution

It introduces a combined Fermi I and Fermi II acceleration model that explains radio relic observations and resolves the Mach number discrepancy issue.

Findings

Fermi I acceleration with fossil electrons reproduces radio profiles.

Shock surfaces may consist of multiple shocks with different Mach numbers.

The model aligns with observed radio spectra of giant relics.

Abstract

According to structure formation simulations, weak shocks with typical Mach number, $M_{\rm s}\lesssim 3$, are expected to form in merging galaxy clusters. The presence of such shocks has been indicated by X-ray and radio observations of many merging clusters. In particular, diffuse radio sources known as radio relics could be explained by synchrotron-emitting electrons accelerated via diffusive shock acceleration (Fermi I) at quasi-perpendicular shocks. Here we also consider possible roles of stochastic acceleration (Fermi II) by compressive MHD turbulence downstream of the shock. Then we explore a puzzling discrepancy that for some radio relics, the shock Mach number inferred from the radio spectral index is substantially larger than that estimated from X-ray observations. This problem could be understood, if shock surfaces associated with radio relics consist of multiple shocks with different strengths.In that case, X-ray observations tend to pick up the part of shocks with lower Mach numbers and higher kinetic energy flux, while radio emissions come preferentially from the part of shocks with higher Mach numbers and higher cosmic ray (CR) production. We also show that the Fermi I reacceleration model with preexisting fossil electrons supplemented by Fermi II acceleration due to postshock turbulence could reproduce observed profiles of radio flux densities and integrated radio spectra of two giant radio relics. This study demonstrates the CR electrons can be accelerated at collisionless shocks in galaxy clusters just like supernova remnant shock in the interstellar medium and interplanetary shocks in the solar wind.