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Cosmological shock waves result from supersonic flow motions induced byhierarchical clustering of nonlinear structures in the universe. These shocksgovern the nature of cosmic plasma through thermalization of gas andacceleration of nonthermal, cosmic-ray (CR) particles. We study the statisticsand energetics of shocks formed in cosmological simulations of a concordance$\Lambda$CDM universe, with a special emphasis on the effects ofnon-gravitational processes such as radiative cooling, photoionization/heating,and galactic superwind feedbacks. Adopting an improved model for gasthermalization and CR acceleration efficiencies based on nonlinear diffusiveshock acceleration calculations, we then estimate the gas thermal energy andthe CR energy dissipated at shocks through the history of the universe. Sinceshocks can serve as sites for generation of vorticity, we also examine thevorticity that should have been generated mostly at curved shocks incosmological simulations. We find that the dynamics and energetics of shocksare governed primarily by the gravity of matter, so other non-gravitationalprocesses do not affect significantly the global energy dissipation andvorticity generation at cosmological shocks. Our results reinforce scenarios inwhich the intracluster medium and warm-hot intergalactic medium containenergetically significant populations of nonthermal particles and turbulentflow motions.

Cosmological Shock Waves in the Large Scale Structure of the Universe: Non-gravitational Effects