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Galaxies form from the accretion of cosmological infall of gas. In the highredshift Universe, most of this gas infall is expected to be dominated by coldfilamentary flows which connect deep down inside halos, and, hence, to thevicinity of galaxies. Such cold flows are important since they dominate themass and angular momentum acquisition that can make up rotationally-supporteddisks at high-redshifts. We study the angular momentum acquisition of gas intogalaxies, and in particular, the torques acting on the accretion flows, usinghydrodynamical cosmological simulations of high-resolution zoomed-in halos of afew $10^{11}\,\rm M_\odot$ at $z=2$. Torques can be separated into those ofgravitational origin, and hydrodynamical ones driven by pressure gradients. Wefind that coherent gravitational torques dominate over pressure torques in thecold phase, and are hence responsible for the spin-down and realignment of thisgas. Pressure torques display small-scale fluctuations of significantamplitude, but with very little coherence on the relevant galaxy or halo-scalethat would otherwise allow them to effectively re-orientate the gas flows. Darkmatter torques dominate gravitational torques outside the galaxy, while withinthe galaxy, the baryonic component dominates. The circum-galactic mediumemerges as the transition region for angular momentum re-orientation of thecold component towards the central galaxy's mid-plane.

Gravitational torques dominate the dynamics of accreted gas at $z>2$