Redshift evolution of the physical radius corresponding to 3R₂₀₀ (≈9 Mpc) surrounding the cluster in the radiative simulation of Halo3. From left to right, we color code the spherically averaged fields of vorticity, metallicity, and magnetic field strength. The upper row shows the redshift range 20 > z > 0.1, highlighting the late time evolution dominated by mergers, while the bottom row shows the redshift range 11 > z > 4, focusing on the evolution in the central galaxy at higher redshifts. The dashed lines indicate the virial radius (R₂₀₀) and the central cluster region (0.25R₂₀₀). We keep the maximum radius in the lower panels at a fixed physical value of 150 kpc (see text). The lower panels show how vorticity and metallicity are enhanced in the center already at high redshifts, z > 9. The central magnetic field amplification sets in shortly afterwards at z ≈ 7. Turbulence from gravitational infall of cool gas amplifies the magnetic field and drives a small-scale dynamo. Stellar feedback additionally injects turbulence, distributes metals, and mixes magnetically enriched gas with less enriched gas. The upper panel highlights how merging substructures contribute their magnetically enriched gas to the host cluster. These merging structures also exhibit higher metallicity, indicating the connection between strong magnetic fields and the metal-rich ISM.