  We revisited the unusual wind in GRO J1655-40 detected with Chandra in 2005
April, using long-term RXTE X-ray data and simultaneous optical/near-infrared
photometric data. This wind is the most convincing case for magnetic driving in
black hole binaries, as it has an inferred launch radius which is a factor of
10 smaller than the thermal wind prediction. However, the optical and
near-infrared fluxes monotonically increase around the Chandra observation,
whereas the X-ray flux monotonically decreases from 10 days beforehand. Yet the
optical and near-infrared fluxes are from the outer, irradiated disk, so for
them to increase implies that the X-rays likewise increased. We applied a new
irradiated disk model to the multi-wavelength spectral energy distributions
(SEDs). Fitting the optical and near-infrared fluxes, we estimated the
intrinsic luminosity at the Chandra epoch was > ~0.7 L_Edd, which is more than
one order of magnitude larger than the observed X-ray luminosity. These results
could be explained if a Compton-thick, almost completely ionized gas was
present in the wind and strong scattering reduced the apparent X-ray
luminosity. The effects of scattering in the wind should then be taken into
account for discussion of the wind-driving mechanism. Radiation pressure and
Compton heating may also contribute to powering the wind at this high
luminosity.
