  Aims: morpholgies, number and energy distributions of Cosmological Shock
Waves from a set of ENZO cosmological simulations are produced, along with a
study of the connection with Cosmic Rays processes in different environments.
Method: we perform cosmological simulations with the public release of the PPM
code ENZO, adopt a simple and physically motivated numerical setup to follow
the evolution of cosmic structures at the resolution of 125kpc per cell, and
characterise shocks with a new post processing scheme. Results: we estimate the
efficency of the acceleration of Cosmic Ray particles and present the first
comparison of our results with existing limits from observations of galaxy
clusters.
