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The injection of turbulence in the circum-galactic medium at redshift z = 2is investigated using the mesh-based hydrodynamic code Enzo and a subgrid-scale(SGS) model for unresolved turbulence. Radiative cooling and heating by auniform Ultraviolet (UV) background are included in our runs and compared withthe effect of turbulence modelling. Mechanisms of gas exchange between galaxiesand the surrounding medium, as well as metal enrichment, are not taken intoaccount, and turbulence is here driven solely by structure formation (mergersand shocks). We find that turbulence, both at resolved and SGS scales, impactsmostly the warm-hot intergalactic medium (WHIM), with temperature between 10^5and 10^7 K, mainly located around collapsed and shock heated structures, and infilaments. Typical values of the ratio of turbulent to thermal pressure is 0.1in the WHIM, corresponding to a volume-weighted average of the SGS turbulent tothermal Doppler broadening b_t / b_therm = 0.26, on length scales below thegrid resolution of 25 kpc/h. In the diffuse intergalactic medium (IGM), definedin a range of baryon overdensity \delta\ between 1 and 50, the importance ofturbulence is smaller, but grows as a function of gas density, and the Dopplerbroadening ratio is fitted by the function b_t / b_therm = 0.023 \delta^{0.58}.

Turbulence driven by structure formation in the circum-galactic medium