  Recent Chandra observations of an outflowing gas in GRO J1655-40 resulted in
a suggestion by Miller et al. (2006) that the wind in this system must be
powered by a magnetic process that can also drive accretion through the disk
around the black hole. The alternative explanations, of radiation pressure or
thermally driven flows, were considered unsatisfactory because of the highly
ionized level of the gas and because of the derived small distance from the
black hole, well inside the minimum distance required for an efficient X-ray
heated wind. The present paper shows that there is a simple photoionized wind
solution for this system where the gas is much further out than assumed by
Miller et al., at r/r_g = 10^(4.7-5.7). The expected wind velocity, as well as
the computed equivalent widths of more than 50 absorption lines in this
single-component 1D model, are all in good agreement with the Chandra
observations.
