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We have designed a simple multi-scale method that identifies turbulentmotions in hydrodynamical grid simulations. The method does not assmume anta-priori coherence scale to distinguish laminar and turbulent flows. Instead,the local mean velocity field around each cell is reconstructed with amulti-scale filtering technique, yielding the maximum scale of turbulent eddiesby means of iterations. The method is robust, fast and easily applicable to anygrid simulation. We present here the application of this technique to the studyof spatial and spectral properties of turbulence in the intra cluster medium,measuring turbulent diffusion and anisotropy of the turbulent velocity fieldfor a variety of driving mechanisms: a) accretion of matter in galaxy clusters(simulated with ENZO); b) sloshing motions around cool-cores (simulated withFLASH); c) jet outflows from active galactic nuclei, AGN (simulated withFLASH). The turbulent velocities driven by matter accretion in galaxy clustersare mostly tangential in the inner regions (inside the cluster virial radius)and isotropic in regions close to the virial radius. The same is found forturbulence excited by cool core sloshing, while the jet outflowing from AGNdrives mostly radial turbulence motions near its sonic point and beyond.Turbulence leads to a diffusivity in the range =10^29-10^30 cm^2/s in the intracluster medium. On average, the energetically dominant mechanism of turbulencedriving in the intra cluster medium is represented by accretion of matter andmajor mergers during clusters evolution.

Turbulence in the ICM from mergers, cool-core sloshing and jets: results from a new multi-scale filtering approach