  X-ray signatures of outflowing gas have been detected in several accreting
black-hole binaries, always in the soft state. A key question raised by these
observations is whether these winds might also exist in the hard state. Here,
we carry out the first full-frequency radiation hydrodynamic simulations of
luminous ($\rm{L = 0.5 \, L_{\mathrm{Edd}}}$) black-hole X-ray binary systems
in both the hard and the soft state, with realistic spectral energy
distributions (SEDs). Our simulations are designed to describe X-ray transients
near the peak of their outburst, just before and after the hard-to-soft state
transition. At these luminosities, it is essential to include radiation
driving, and we include not only electron scattering, but also photoelectric
and line interactions. We find powerful outflows with $\rm{\dot{M}_{wind}
\simeq 2 \,\dot{M}_{acc}}$ are driven by thermal and radiation pressure in both
hard and soft states. The hard-state wind is significantly faster and carries
approximately 20 times as much kinetic energy as the soft-state wind. However,
in the hard state the wind is more ionized, and so weaker X-ray absorption
lines are seen over a narrower range of viewing angles. Nevertheless, for
inclinations $\gtrsim 80^{\circ}$, blue-shifted wind-formed Fe XXV and Fe XXVI
features should be observable even in the hard state. Given that the data
required to detect these lines currently exist for only a single system in a
{\em luminous} hard state -- the peculiar GRS~1915+105 -- we urge the
acquisition of new observations to test this prediction. The new generation of
X-ray spectrometers should be able to resolve the velocity structure.
