  We apply the disk-corona evaporation model (Meyer & Meyer-Hofmeister)
originally derived for dwarf novae to black hole systems. This model describes
the transition of a thin cool outer disk to a hot coronal flow. The mass
accretion rate determines the location of this transition. For a number of well
studied black hole binaries we take the mass flow rates derived from a fit of
the ADAF model to the observed spectra (for a review see Narayan, Mahadevan, &
Quataert) and determine where the transition of accretion via a cool disk to a
coronal flow/ADAF would be located for these rates. We compare with the
observed location of the inner disk edge, as estimated from the maximum
velocity of the $\rm H_\alpha$ emission line. We find that the transition
caused by evaporation agrees with this in stellar disks. We also show that the
ADAF and the ``thin outer disk + corona'' are compatible in terms of the
physics in the transition region.
