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Ubiquitous detections of cold/warm gas around galaxies indicate that thecircumgalactic medium (CGM) is multiphase and dynamic. Recent state-of-the-artcosmological galaxy simulations have generally underproduced the column densityof cold halo gas. We argue that this may be due to a mismatch of spatialresolution in the circumgalactic space and the relevant physical scales atwhich the cold gas operates. Using semi-analytic calculations and a set ofmagnetohydrodynamic (MHD) simulations, we present a multiphase model of thegaseous halos around galaxies, the circumgalactic mist (CGm). The CGm model isbased on the idea that the observed cold halo gas may be a composite of cold,dense and small cloudlets embedded in a hot diffuse halo, resemblingterrestrial clouds and mist. We show that the resulting cold gas from thermalinstabilities conforms to a characteristic column density of $N_{\rm H}\approx10^{17}\rm{cm^{-2}}$ as predicted by the $c_s t_{\rm cool}$ ansatz. The modelimplies a large number of cold clumps in the inner galactic halo with a smallvolume filling factor but large covering fraction. The model also naturallygives rise to spatial extents and differential covering fractions of cold, warmand hot gas. To self-consistently model the co-evolution of the CGM and starformation within galaxies, future simulations must address the mismatch of thespatial resolution and characteristic scale of cold gas.

On the model of the circumgalactic mist: the implications of cloud sizes in galactic winds and halos