Exploring the role of accretion shocks in galaxy clusters as sources of ultrahigh-energy cosmic rays

TL;DR

This study explores whether accretion shocks in galaxy clusters can accelerate ultrahigh-energy cosmic rays, fitting observational data to assess their contribution to the cosmic ray flux and composition.

Contribution

It introduces a model linking galaxy cluster accretion shocks to UHECR acceleration, fitting flux and composition data to evaluate their significance as sources.

Findings

Accretion shocks may explain a fraction of observed UHECRs below the energy suppression.

Higher energies require exceptional conditions like stronger magnetic fields or specific shock configurations.

The model aligns with Pierre Auger Observatory data on cosmic ray flux and composition.

Abstract

Recently, the Pierre Auger Observatory has found strong evidence supporting the extragalactic origin of the most energetic cosmic rays. Despite several observed excesses in the distribution of arrival directions for the highest energy cosmic rays, the sources remain unidentified. Accretion shocks in galaxy clusters have been proposed as potential sources in the past. These immense shock waves, which can have radii on the order of megaparsecs, are generated by the infall of material from the intergalactic medium into the gravitational potential wells of galaxy clusters. In this work, we investigate the possibility that ultrahigh-energy cosmic rays are accelerated in these regions. Nearby massive galaxy clusters, including Virgo, are treated as a discrete component of the cluster mass distribution. Less massive galaxy clusters, as well as distant massive ones, are assumed to follow a continuous distribution in agreement with cluster mass statistics. We fit the flux at Earth and the composition profile measured by the Pierre Auger Observatory, assuming the injection of different nuclear species by these sources, to determine the values of the model parameters. Our results indicate that cosmic ray acceleration in cluster accretion shocks may account for at least a fraction of the observed UHECR flux at energies below the suppression scale. At higher energies, direct acceleration from the thermal pool would be feasible only if local fluctuations create favorable conditions, such as magnetic fields about an order of magnitude stronger than those typically expected in cluster accretion shocks, or for particular shock normal-magnetic field configurations.