  Galaxy clusters are the largest gravitationally-bound structures in the
Universe. As such, during merger events with similar systems, they release an
enormous amount of energy that is dissipated through the formation of shock
waves and turbulence in the intracluster medium (ICM), the hot ionised plasma
permeating the cluster volume. These shock waves are believed to be ideal sites
for electron acceleration that, in the presence of ubiquitous magnetic fields
in the ICM, are capable of producing elongated non-thermal radio features
typically observed in the outskirts of dynamically disturbed clusters, also
known as radio relics. In this work, we analyse a hydrodynamical re-simulation
of merging galaxy clusters, extracted from a large set of zoom-in cosmological
simulations of The Three Hundred Project, to study the evolution and diversity
of merger shocks and their associated diffuse radio emission within the
framework of the diffusive shock acceleration scenario.
