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We explore the poloidal structure of two-dimensional (2D) MHD winds inrelation to their potential association with the X-ray warm absorbers (WAs) andthe highly-ionized ultra-fast outflows (UFOs) in AGN, in a single unifyingapproach. We present the density $n(r,\theta)$, ionization parameter$\xi(r,\theta)$, and velocity structure $v(r,\theta)$ of such ionized winds fortypical values of their fluid-to-magnetic flux ratio, $F$, and specific angularmomentum, $H$, for which wind solutions become super-\Alfvenic. We explore thegeometrical shape of winds for different values of these parameters anddelineate the values that produce the widest and narrowest opening angles ofthese winds, quantities necessary in the determination of the statistics of AGNobscuration. We find that winds with smaller $H$ show a poloidal geometry ofnarrower opening angles with their \Alfven\ surface at lower inclination anglesand therefore they produce the highest line of sight (LoS) velocities forobservers at higher latitudes with the respect to the disk plane. We furthernote a physical and spatial correlation between the X-ray WAs and UFOs thatform along the same LoS to the observer but at different radii, $r$, anddistinct values of $n$, $\xi$ and $v$ consistent with the latest spectroscopicdata of radio-quiet Seyfert galaxies. We also show that, at least in the caseof 3C 111, the winds' pressure is sufficient to contain the relativistic plasmaresponsible for its radio emission. Stratified MHD disk-winds could thereforeserve as a unique means to understand and unify the diverse AGN outflows.

Stratified Magnetically-Driven Accretion-Disk Winds and Their Relations to Jets