Exploring the role of cosmological shock waves in the Dianoga
  simulations of galaxy clusters
  Cosmological shock waves are ubiquitous to cosmic structure formation and
evolution. As a consequence, they play a major role in the energy distribution
and thermalization of the intergalactic medium (IGM). We analyze the Mach
number distribution in the Dianoga simulations of galaxy clusters performed
with the SPH code GADGET-3. The simulations include the effects of radiative
cooling, star formation, metal enrichment, supernova and active galactic nuclei
feedback. A grid-based shock-finding algorithm is applied in post-processing to
the outputs of the simulations. This procedure allows us to explore in detail
the distribution of shocked cells and their strengths as a function of cluster
mass, redshift and baryonic physics. We also pay special attention to the
connection between shock waves and the cool-core/non-cool core (CC/NCC) state
and the global dynamical status of the simulated clusters. In terms of general
shock statistics, we obtain a broad agreement with previous works, with weak
(low-Mach number) shocks filling most of the volume and processing most of the
total thermal energy flux. As a function of cluster mass, we find that massive
clusters seem more efficient in thermalising the IGM and tend to show larger
external accretion shocks than less massive systems. We do not find any
relevant difference between CC and NCC clusters. However, we find a mild
dependence of the radial distribution of the shock Mach number on the cluster
dynamical state, with disturbed systems showing stronger shocks than regular
ones throughout the cluster volume.
