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We present the first results of one extremely high resolution, non-radiativemagnetohydrodynamical cosmological zoom-in simulation of a massive cluster witha virial mass M$_\mathrm{vir} = 2.0 \times 10^{15}$ solar masses. We adopt amass resolution of $4 \times 10^5$ M$_{\odot}$ with a maximum spatialresolution of around 250 pc in the central regions of the cluster. We followthe detailed amplification process in a resolved small-scale turbulent dynamoin the Intracluster medium (ICM) with strong exponential growth until redshift4, after which the field grows weakly in the adiabatic compression limit untilredshift 2. The energy in the field is slightly reduced as the systemapproaches redshift zero in agreement with adiabatic decompression. The fieldstructure is highly turbulent in the center and shows field reversals on alength scale of a few 10 kpc and an anti-correlation between the radial andangular field components in the central region that is ordered by small-scaleturbulent dynamo action. The large-scale field on Mpc scales is almostisotropic, indicating that the structure formation process in massive galaxycluster formation is suppressing memory of both the initial field configurationand the amplified morphology via the turbulent dynamo in the central regions.We demonstrate that extremely high-resolution simulations of the magnetized ICMare in reach that can resolve the small-scale magnetic field structure which isof major importance for the injection of and transport of cosmic rays in theICM. This work is a major cornerstone for follow-up studies with an on-the-flytreatment of cosmic rays to model in detail electron-synchrotron and gamma-rayemissions.

Towards cosmological simulations of the magnetized intracluster medium with resolved Coulomb collision scale