  Observations of X-ray absorption lines in magnetically driven disk winds
around black hole binaries and active galactic nuclei yield a universal radial
density profile rho proportional to r^{-1.2} in the wind. This is in
disagreement with the standard Blandford & Payne profile rho_BP proportional to
r^{-1.5} expected when the magnetic field is neither advected nor diffusing
through the accretion disk. In order to account for this discrepancy, we
establish a new paradigm for magnetically driven astrophysical winds according
to which the large scale ordered magnetic field that threads the disk is
continuously generated by the Cosmic Battery around the inner edge of the disk
and continuously diffuses outward. We obtain self-similar solutions of such
magnetically advected winds (MAW) and discuss their observational
ramifications.
