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 { L _ { Edd } } .
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 .