  Hydrostatic equilibrium (HSE), where the thermal pressure gradient balances
the force of gravity, is tested across a range of simulated EAGLE haloes from
Milky Way L* haloes (M_200~10^12 Msol) to cluster scales. Clusters
(M_200>=10^14 Msol) reproduce previous results with thermal pressure
responsible for ~90% of the support against gravity, but this fraction drops
for 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 the
binding energy of a halo toward lower mass resulting in greater deviations from
HSE. Tangential motions comprise the largest deviation from HSE in L* haloes
indicating that the hot circumgalactic medium (CGM) has significant sub-
centrifugal rotation and angular momentum spin parameters 2-3x higher than the
dark matter spin parameters. Thermal feedback can buoyantly rise to the outer
CGM of M_200<10^12 Msol haloes, both moving baryons beyond R_200 and feeding
uncorrelated tangential motions. The resulting hot halo density and rotation
profiles show promising agreement with X-ray observations of the inner Milky
Way halo, and we discuss future observational prospects to detect spinning hot
haloes around other galaxies. Acceleration and radial streaming motions also
comprise significant deviations from HSE, especially net outward accelerations
seen in L* and group haloes indicating active feedback. Black hole feedback
acts in a preventative manner during the later growth of group haloes, applying
significant accelerations via shocks that do not feed tangential motions. We
argue that HSE is a poor assumption for the CGM, especially in the inner
regions, and rotating baryonic hot haloes are a critical consideration for
analytic models of the CGM.
