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Massive structures like cluster of galaxies, embedded in cosmic filaments,release enormous amount of energy through their interactions. These events areassociated with production of Mpc-scale shocks and injection of considerableamount of turbulence, affecting the non-thermal energy budget of the ICM. Inorder to study this thoroughly, we performed a set of cosmological simulationsusing the hydrodynamical code Enzo. We studied the formation of clustersundergoing major mergers, the propagation of merger shocks and theirinteraction with the filamentary cosmic web. This interaction is shown toproduce peripheral structures remarkably similar to giant radio relicsobserved, for example, in Abell 3376 and Abell 3667. We find a relatively longtimescale (about 4 Gyr) for turbulence decay in the centre of major mergingclusters. This timescale is substantially longer than typically assumed in theturbulent re-acceleration models, invoked for explaining the statistics ofobserved radio halos.

Evolution of shocks and turbulence in the formation of galaxy clusters embedded in Megaparsec-scale filaments