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Theory and simulations suggest that magnetic fields from radio jets and lobespowered by their central super massive black holes can be an important sourceof magnetic fields in the galaxy clusters. This is paper II in a series ofstudies where we present self-consistent high-resolution adaptive meshrefinement cosmological magnetohydrodynamic (MHD) simulations thatsimultaneously follow the formation of a galaxy cluster and evolution ofmagnetic fields ejected by an active galactic nucleus (AGN). We studied 12different galaxy clusters with virial masses ranging from 1 $\times$ 10$^{14}$to 2 $\times$ 10$^{15}$ M$_{\odot}$. In this work we examine the effects of themass and merger history on the final magnetic properties. We find that theevolution of magnetic fields is qualitatively similar to those of previousstudies. In most clusters, the injected magnetic fields can be transportedthroughout the cluster and be further amplified by the intra-cluster medium(ICM) turbulence during the cluster formation process with hierarchicalmergers, while the amplification history and the magnetic field distributiondepend on the cluster formation and magnetism history. This can be verydifferent for different clusters. The total magnetic energies in these clustersare between 4 $\times$ 10$^{57}$ and $10^{61}$ erg, which is mainly decided bythe cluster mass, scaling approximately with the square of the total mass.Dynamically older relaxed clusters usually have more magnetic fields in theirICM. The dynamically very young clusters may be magnetized weakly since thereis not enough time for magnetic fields to be amplified.

Evolution and Distribution of Magnetic Fields from AGNs in Galaxy Clusters II. The Effects of Cluster Size and Dynamical State