  We extend our modeling of the ionization structure of magnetohydrodynamic
(MHD) accretion-disk winds, previously applied to Seyfert galaxies, to a
population of quasi-stellar-objects (QSOs) of much lower X-ray-to-UV flux
ratios, i.e. smaller $\alpha_{\rm ox}$ index, motivated by UV/X-ray ionized
absorbers with extremely high outflow velocities in UV-luminous QSOs. We
demonstrate that magnetically-driven winds ionized by a spectrum with
$\alpha_{\rm ox} \simeq -2$ can produce the charge states responsible for \civ
~and \fexxv/\fexxvi ~absorption in wind regions with corresponding maximum
velocities of $v$(\civ) $\lsim 0.1c$ and $v({\rm \fexxv}) \lsim 0.6 c$ (where
$c$ is the speed of light) and column densities $N_H \sim 10^{23}-10^{24}$
cm$^{-2}$, in general agreement with observations. In contrast to the
conventional radiation-driven wind models, {\it high-velocity flows are always
present in our MHD-driven winds} but manifest in the absorption spectra only
for $\alpha_{\rm ox} \lsim -2$, as larger $\alpha_{\rm ox}$ values ionize the
wind completely out to radii too large to demonstrate the presence of these
high velocities. We thus predict increasing velocities of these ionized
absorbers with decreasing (steeper) $\alpha_{\rm ox}$, a quantity that emerges
as the defining parameter in the kinematics of the AGN UV/X-ray absorbers.
