On the small scale turbulent dynamo in the intracluster medium: A comparison to dynamo theory

Understand

We present non-radiative, cosmological zoom-simulations of galaxy cluster formation with magnetic fields and (anisotropic) thermal conduction of one very massive galaxy cluster with a mass at redshift zero that corresponds to $M_\mathrm{vir} \sim 2 \times 10^{15} M_{\odot}$.

• We run the cluster on three resolution levels (1X, 10X, 25X), starting with an effective mass resolution of $2 \times 10^8M_{\odot}$, subsequently increasing the particle number to reach $4 \times 10^6M_{\odot}$.
• The maximum spatial resolution obtained in the simulations is limited by the gravitational softening reaching $\epsilon=1.0$ kpc at the highest resolution level, allowing to resolve the hierarchical assembly of the structures in very fine detail.
• All simulations presented, have been carried out with the SPMHD-code Gadget-3 with a heavily updated SPMHD prescription.