  We present a unified model for the structure and appearance of accretion
powered sources across their entire luminosity range from galactic X-ray
binaries to luminous quasars, with emphasis on AGN and their phenomenology.
Central to this model is the notion of MHD winds launched from the accretion
disks that power these objects. These winds provide the matter that manifests
as blueshifted absorption features in the UV and X-ray spectra of a large
fraction of these sources; furthermore, their density distribution in the
poloidal plane determines the "appearance" (i.e. the column and velocity
structure of these absorption features) as a function of the observer
inclination angle. This work focuses on just the broadest characteristics of
these objects; nonetheless, it provides scaling laws that allow one to
reproduce within this model the properties of objects spanning a very wide
luminosity range and viewed at different inclination angles, and trace them to
a common underlying dynamical structure. Its general conclusion is that the AGN
phenomenology can be accounted for in terms of three parameters: The wind mass
flux in units of the Eddington value, $\dot m$, the observer's inclination
angle $\theta$ and the logarithmic slope between the O/UV and X-ray fluxes
$\alpha_{OX}$. However, because of a significant correlation between
$\alpha_{OX}$ and UV luminosity, we conclude that the AGN structure depends on
only two parameters. Interestingly, the correlations implied by this model
appear to extend to and consistent with the characteristics of galactic X-ray
sources, suggesting the presence of a truly unified underlying structure for
accretion powered sources.
