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Observed accretion rates onto the Milky-Way and other local spirals fallshort of that required to sustain star formation for cosmological timescales. Apotential avenue for this unseen accretion is an inflow in the volume-fillinghot phase ($\sim10^6$ K) of the circumgalactic medium (CGM), as suggested bysome cosmological simulations. We derive an approximate axisymmetric analyticsolution of such hot CGM accretion flows, and validate it with hydrodynamicsimulations. We show that a hot inflow spins up as it approaches the galaxy,while remaining hot, subsonic and quasi-spherical. At the radius of angularmomentum support ($\approx15$ kpc for the Milky-Way) the hot flow flattens intoa disk geometry and then cools from $\sim10^6$ K to $\sim10^4$ K at thedisk-halo interface. Cooling affects all hot gas, rather than just a subset ofindividual gas clouds, implying that accretion via hot inflows does not rely onlocal thermal instability in contrast with 'precipitation' models for galaxyaccretion. Prior to cooling and accretion the inflow completes $\sim t_{\rmcool}/t_{\rm ff}$ radians of rotation, where $t_{\rm cool}/t_{\rm ff}$ is thecooling time to free-fall time ratio in hot gas immediately outside the galaxy.The ratio $t_{\rm cool}/t_{\rm ff}$ may thus govern the development ofturbulence and enhancement of magnetic fields in gas accreting ontolow-redshift spirals. We argue that accretion via hot inflows can explain theobserved truncation of nearby thin stellar disks at $\approx4$ disk radii. Wealso show that if rotating hot inflows are common in Milky-Way size diskgalaxies, as predicted, then signatures should be observable with X-raytelescopes, kinetic SZ measurements, and FRB surveys.

Accretion onto disk galaxies via hot and rotating CGM inflows