  We present an analytic description of turbulent, MHD disk accretion around
black holes that specifically addresses the relationship between radial and
vertical, transport, thereby complementing and extending numerical simulations.
The azimuthal-vertical component of the magnetic stress is fundamental to an
understanding of disk--corona--outflow coupling: when it is important for
driving the angular momentum transport and mass accretion in the disk, it also
has an important influence on the disk--corona--outflow energy budget. The
Poynting flux derived from the product of this term with the Keplerian velocity
dominates the Poynting flux into the corona. The ratio of the coronal Alfven
velocity to the Keplerian velocity is an important parameter. If this parameter
is greater than unity then energetically significant winds and Poynting flux
into the corona occur. However, significant effects could occur when this
parameter is much less than unity. A limiting solution describing the case of
angular momentum transport solely by the vertical-azimuthal stress features all
of the accretion power being channeled into a wind, some of which would be
dissipated in the corona. More realistic solutions in which there is both
radial and vertical transport of angular momentum would have different
fractions of the accretion power emitted by the disk and corona. These results
have important implications for existing accretion disk theory and for our
interpretation of high-energy emission and nuclear outflows from black holes.
