  A number of X-ray binaries exhibit clear evidence for the presence of disk
winds in the high/soft state. A promising driving mechanism for these outflows
is mass loss driven by the thermal expansion of X-ray heated material in the
outer disk atmosphere. Higginbottom \& Proga recently demonstrated that the
properties of thermally-driven winds depend critically on the shape of the
thermal equilibrium curve, since this determines the thermal stability of the
irradiated material. For a given spectral energy distribution, the thermal
equilibrium curve depends on exact balance between the various heating and
cooling mechanisms at work. Most previous work on thermally-driven disk winds
relied an analytical approximation to these rates. Here, we use the
photoionization code \textsc{cloudy} to generate realistic heating and cooling
rates which we then use in a 2.5D hydrodynamic model computed in ZEUS to
simulate thermal winds in a typical black-hole X-ray binary. We find that these
heating and cooling rates produce a significantly more complex thermal
equilibrium curve, with dramatically different stability properties. The
resulting flow, calculated in the optically thin limit, is qualitatively
different from flows calculated using approximate analytical rates.
Specifically, our thermal disk wind is much denser and slower, with a mass-loss
rate that is a factor of two higher and characteristic velocities that are a
factor of three lower. The low velocity of the flow -- $v_{max} \simeq
200$~km~s$^{-1}$ -- may be difficult to reconcile with observations. However,
the high mass-loss rate -- 15$\times$ the accretion rate -- is promising, since
it has the potential to destabilize the disk. Thermally-driven disk winds may
therefore provide a mechanism for state changes.
