  We present a generally applicable formalism for modeling the emission,
absorption, reflection, and reprocessing of radiation by moving plasma streams
close to a Kerr Black hole. The formalism can be used to investigate the
observational signatures of a wide range of phenomena, including: (i) the
reflection of coronal X-ray radiation off plasma plunging from the inner edge
of a black hole accretion disk towards the black hole; (ii) the reflection of
coronal X-ray emission off the upper layers of a geometrically thick accretion
flow; (iii) the illumination of the accretion disk by a corona moving with
relativistic velocities towards or away from the accretion disk; (iv) the
emission from a jet forming close to the black hole. After introducing the
general relativistic treatment, we show the results for a fast wind forming
close to a Kerr black hole. The approach presented here can be used to model
X-ray spectral, timing, reverberation, and polarization data.
