  During structure formation, energetic events and random motions of the hot
gas residing inside galaxy clusters (the intracluster medium, ICM) generate
turbulent motions. Radio diffuse emission probes the presence of magnetic
fields and relativistic particles in the ICM, being a key ingredient for
understanding the physical processes at work in clusters of galaxies. In this
work, we present results from numerical simulations of magnetic field
turbulence in magnetohydrodynamics (MHD) and kinetic MHD (KMHD) frameworks. We
characterize magnetic field structures through the imprints left on
polarization maps.
