  The mechanisms that drive disk winds are a window into the physical processes
that underlie the disk. Stellar-mass black holes are an ideal setting in which
to explore these mechanisms, in part because their outbursts span a broad range
in mass accretion rate. We performed a spectral analysis of the disk wind found
in six Chandra/HETG observations of the black hole candidate 4U~1630$-$472,
covering a range of luminosities over two distinct spectral states. We modeled
both wind absorption and extended wind re-emission components using PION, a
self-consistent photoionized absorption model. In all but one case, two
photoionization zones were required in order to obtain acceptable fits. Two
independent constraints on launching radii, obtained via the ionization
parameter formalism and the dynamical broadening of the re-emission, helped
characterize the geometry of the wind. The innermost wind components ($r \simeq
{10}^{2-3}$ $GM/{c}^{2}$) tend towards small volume filling factors, high
ionization, densities up to $n \simeq {10}^{15-16} {\text{cm}}^{-3}$, and
outflow velocities of $\sim 0.003c$. These small launching radii and large
densities require magnetic driving, as they are inconsistent with numerical and
analytical treatments of thermally driven winds. Outer wind components ($r
\simeq {10}^{5}$ $GM/{c}^{2}$) are significantly less ionized and have filling
factors near unity. Their larger launching radii, lower densities ($n \simeq
{10}^{12} {\text{cm}}^{-3}$), and outflow velocities ($\sim 0.0007c$) are
nominally consistent with thermally driven winds. The overall wind structure
suggests that these components may also be part of a broader MHD outflow and
perhaps better described as magneto-thermal hybrid winds.
