  We present an analysis of ionized X-ray disk winds observed in the Fe K band
of four stellar-mass black holes observed with Chandra, including 4U 1630-47,
GRO J1655-40, H 1743-322, and GRS 1915+105. High-resolution photoionization
grids were generated in order to model the data. Third-order gratings spectra
were used to resolve complex absorption profiles into atomic effects and
multiple velocity components. The Fe XXV line is found to be shaped by
contributions from the intercombination line (in absorption), and the Fe XXVI
line is detected as a spin-orbit doublet. The data require 2-3 absorption
zones, depending on the source. The fastest components have velocities
approaching or exceeding 0.01c, increasing mass outflow rates and wind kinetic
power by orders of magnitude over prior single-zone models. The first-order
spectra require re-emission from the wind, broadened by a degree that is
loosely consistent with Keplerian orbital velocities at the photoionization
radius. This suggests that disk winds are rotating with the orbital velocity of
the underlying disk, and provides a new means of estimating launching radii --
crucial to understanding wind driving mechanisms. Some aspects of the wind
velocities and radii correspond well to the broad-line region (BLR) in active
galactic nuclei, suggesting a physical connection. We discuss these results in
terms of prevalent models for disk wind production and disk accretion itself,
and implications for massive black holes in active galactic nuclei.
