In this lecture I present our recent results of characterizing cosmological shocks within adaptive mesh refinement N-body/hydrodynamic simulations that are used to predict non-thermal components of large-scale structure. We propose a modified algorithm for finding shocks from those used on unigrid simulations that reduces the shock frequency of low Mach number shocks by a factor of ~3. We then apply our new technique to a large, (512 h⁻¹ Mpc)³, cosmological volume and study the shock Mach number ([Mscr ]) distribution as a function of pre-shock temperature, density, and redshift. We find that the Mach number evolution can be interpreted as a method to visualize large-scale structure formation. By applying results from nonlinear diffusive shock acceleration models using the first-order Fermi process, we calculate the amount of kinetic energy that is converted into cosmic ray protons.