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Speaker: Klaus Dolag, Max Planck Institute for Astronomy
Abstract: In galaxy clusters, non-thermal components such as magnetic field and high energy particles keep a record of the processes acting since early times till now. These components play key roles by controlling transport processes inside the cluster atmosphere and therefore have to be understood in detail. However including them in simulations is extremely challenging as the structures in and around clusters are quite complex and span a very large dynamic range in scales. I will report the status of what can be achieved in numerical simulations of the formation of galaxy clusters in cosmological context and our predictions for the magnetic field structure for different models of magnetic seed fields. This allows us to put constrains on the presence of cosmic ray protons in galaxy clusters by comparing in detail the induced radio emission in these simulations with observations. Additional, such simulations can be used to constrain the transport and the deflection of UHECRs within clusters and large scale structures.