  We explore the poloidal structure of two-dimensional (2D) MHD winds in
relation to their potential association with the X-ray warm absorbers (WAs) and
the highly-ionized ultra-fast outflows (UFOs) in AGN, in a single unifying
approach. We present the density $n(r,\theta)$, ionization parameter
$\xi(r,\theta)$, and velocity structure $v(r,\theta)$ of such ionized winds for
typical values of their fluid-to-magnetic flux ratio, $F$, and specific angular
momentum, $H$, for which wind solutions become super-\Alfvenic. We explore the
geometrical shape of winds for different values of these parameters and
delineate the values that produce the widest and narrowest opening angles of
these winds, quantities necessary in the determination of the statistics of AGN
obscuration. We find that winds with smaller $H$ show a poloidal geometry of
narrower opening angles with their \Alfven\ surface at lower inclination angles
and therefore they produce the highest line of sight (LoS) velocities for
observers at higher latitudes with the respect to the disk plane. We further
note a physical and spatial correlation between the X-ray WAs and UFOs that
form along the same LoS to the observer but at different radii, $r$, and
distinct values of $n$, $\xi$ and $v$ consistent with the latest spectroscopic
data of radio-quiet Seyfert galaxies. We also show that, at least in the case
of 3C 111, the winds' pressure is sufficient to contain the relativistic plasma
responsible for its radio emission. Stratified MHD disk-winds could therefore
serve as a unique means to understand and unify the diverse AGN outflows.
