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Hydrostatic equilibrium (HSE), where the thermal pressure gradient balancesthe force of gravity, is tested across a range of simulated EAGLE haloes fromMilky Way L* haloes (M_200~10^12 Msol) to cluster scales. Clusters(M_200>=10^14 Msol) reproduce previous results with thermal pressureresponsible for ~90% of the support against gravity, but this fraction dropsfor group-sized haloes (M_200~10^13 Msol) and is even lower (40-70%) for L*haloes between 0.1-0.3 R_200. Energy from feedback grows relative to thebinding energy of a halo toward lower mass resulting in greater deviations fromHSE. Tangential motions comprise the largest deviation from HSE in L* haloesindicating that the hot circumgalactic medium (CGM) has significant sub-centrifugal rotation and angular momentum spin parameters 2-3x higher than thedark matter spin parameters. Thermal feedback can buoyantly rise to the outerCGM of M_200<10^12 Msol haloes, both moving baryons beyond R_200 and feedinguncorrelated tangential motions. The resulting hot halo density and rotationprofiles show promising agreement with X-ray observations of the inner MilkyWay halo, and we discuss future observational prospects to detect spinning hothaloes around other galaxies. Acceleration and radial streaming motions alsocomprise significant deviations from HSE, especially net outward accelerationsseen in L* and group haloes indicating active feedback. Black hole feedbackacts in a preventative manner during the later growth of group haloes, applyingsignificant accelerations via shocks that do not feed tangential motions. Weargue that HSE is a poor assumption for the CGM, especially in the innerregions, and rotating baryonic hot haloes are a critical consideration foranalytic models of the CGM.

Deviations from hydrostatic equilibrium in the circumgalactic medium: spinning hot haloes and accelerating flows