  Relativistic emission lines generated by thin accretion disks around rotating
black holes are an important diagnostic tool for testing gravity near the
horizon. The iron K-line is of special importance for the interpretation of the
X-ray emission of Seyfert galaxies, quasars and galactic X-ray binary systems.
A generalized kinematic model is presented which includes radial drifts and
non-Keplerian rotations for the line emitters. The resulting line profiles are
obtained with an object-oriented ray tracer operating in the curved Kerr
background metric. The general form of the Doppler factor is presented which
includes all kinds of poloidal and toroidal motions near the horizon. The
parameters of the model include the spin parameter, the inclination, the
truncation and outer radius of the disk, velocity profiles for rotation and
radial drift, the emissivity profile and a multi-species line-system. The red
wing flux is generally reduced when radial drift is included as compared to the
pure Keplerian velocity field. All resulting emission line profiles can be
classified as triangular, double-horned, double-peaked, bumpy and
shoulder-like. Of particular interest are emission line profiles generated by
truncated standard accretion disks (TSD). It is also shown that the emissivity
law has a great influence on the profiles. The characteristic shoulder-like
line profile observed for the Seyfert galaxy MCG-6-30-15 can be reproduced for
suitable parameters
