  The condensation of matter from a corona to a cool, optically thick inner
disk is investigated for black hole X-ray transient systems in the low hard
state. A description of a simple model for the exchange of energy and mass
between corona and disk originating from thermal conduction is presented,
taking into account the effect of Compton cooling of the corona by photons from
the underlying disk. It is found that a weak, condensation-fed inner disk can
be present in the low hard state of black hole transient systems for a range of
luminosities which depend on the magnitude of the viscosity parameter. For
$\alpha \sim 0.1-0.4$ an inner disk can exist for luminosities in the range
$\sim 0.001- 0.02$ Eddington value. The model is applied to the X-ray
observations of the black hole candidate sources GX 339-4 and Swift
J1753.5-0127 in their low hard state. It is found that Compton cooling is
important in the condensation process, leading to the maintenance of cool inner
disks in both systems. As the results of the evaporation/condensation model are
independent of the black hole mass, it is suggested that such inner cool disks
may contribute to the optical and ultraviolet emission of low luminosity active
galactic nuclei.
