Radio emission of galaxy clusters

We use a simplified numerical model for the relativistic electron population originating from hadronic proton decays inside a galaxy cluster to calculate its characteristic radio synchrotron emission under the influence of strong accretion and merger shocks. Earlier investigations showed that during structure formation the ICM magnetic field can be substantially magnified.We therefore expect the cluster dynamics to manifest itself in the observable synchrotron emission. Comparison to observations will help us gain better insight into the physics of cluster formation. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)