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Merger and non-merger galaxy clusters in cosmological AMR simulations

Aims: We discuss the dependence of shocks, cosmic rays acceleration and turbulence on the dynamical state of the host clusters. Method: We perform cosmological simulations with the grid code ENZO 1.5, with a mesh refinement scheme tailored to follow at high resolution shocks and turbulence developed in the clusters volume. Results: Sizable differences are found when some important properties, connected to non-thermal activity in clusters, are compared for post-merger, merging and relaxing systems.

preprint2011arXivOpen access
Franco Vazza
astro-ph.CO
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Franco Vazza

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