  We analyze three prototypical black hole (BH) X-ray binaries (XRBs), \4u1630,
\gro1655\ and \h1743, in an effort to systematically understand the intrinsic
state transition of the observed accretion-disk winds between \windon\ and
\windoff\ states by utilizing state-of-the-art {\it Chandra}/HETGS archival
data from multi-epoch observations. We apply our magnetically-driven wind
models in the context of magnetohydrodynamic (MHD) calculations to constrain
their (1) global density slope ($p$), (2) their density ($n_{17}$) at the foot
point of the innermost launching radius and (3) the abundances of heavier
elements ($A_{\rm Fe,S,Si}$). Incorporating the MHD winds into {\tt xstar}
photoionization calculations in a self-consistent manner, we create a library
of synthetic absorption spectra given the observed X-ray continua. Our analysis
clearly indicates a characteristic bi-modal transition of multi-ion X-ray
winds; i.e. the wind density gradient is found to steepen (from $p \sim
1.2-1.4$ to $\sim 1.4-1.5$) while its density normalization declines as the
source transitions from \windon\ to \windoff\ state. The model implies that the
ionized wind {\it remains physically present} even in \windoff\ state, despite
its absent appearance in the observed spectra. Super-solar abundances for
heavier elements are also favored. Our global multi-ion wind models, taking
into account soft X-ray ions as well as Fe K absorbers, show that the internal
wind condition plays an important role in wind transitions besides
photoionization changes. % Simulated {\it XRISM}/Resolve and {\it Athena}/X-IFU
spectra are presented to demonstrate a high fidelity of the multi-ion wind
model for better understanding of these powerful ionized winds in the coming
decades.
