  In the inner-most regions of radiation pressure supported accretion disks,
the turbulent magnetic pressure may greatly exceed that of the gas. If this is
the case, it is possible for bulk Alfvenic motions driven by the
magnetorotational instability (MRI) to surpass the electron thermal velocity.
Bulk rather than thermal Comptonization may then be the dominant radiative
process which mediates gravitational energy release. For sufficiently large
turbulent stresses, we show that turbulent Comptonization produces a
significant contribution to the far-UV and X-ray emission of black hole
accretion disks. The existence of this spectral component provides a means of
obtaining direct observational constraints on the nature of the turbulence
itself. We describe how this component may affect the spectral energy
distributions and variability properties of X-ray binaries and active galactic
nuclei.
