Ludwig M. Böss | Galaxy Cluster simulations with a spectral Cosmic ray model
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Europe/Berlin
SR 05 (Villa)
SR 05
Villa
Description
In the large scale structure of the Universe, Galaxy Clusters make up the largest gravitationally bound structures.
The collisions of Galaxy Clusters dissipates a large fraction of their gravitational energy in the form of shock waves which heat the intra-cluster medium to keV energies and can accelerate protons and electrons to relativistic velocities.
Non-thermal emission from relativistic electrons gives insight into the strength and morphology of intra-cluster magnetic fields, as well as providing powerful tracers of structure formation shocks.
Diffuse gamma-ray emission caused by CR protons on the other hand still challenges current observations and is therefore testing models of proton acceleration at intra-cluster shocks.
Large-scale simulations including the effects of CRs have been difficult to achieve since the difference between the scale where CRs interact with the thermal gas and the resolution of these simulations spans more than 20 orders of magnitude.
In this talk I will give an overview of how we try to improve on the modeling of CRs in our large-scale simulations of massive galaxy clusters by adding populations of CRs to each resolution element of the simulation and evolving these populations in time.
This allows us to reproduce observations of radio relics and make predictions for CR electron populations within the cluster volume, as well as potential diffuse gamma-ray emission caused by CR protons.
