  Recent observations have shown that the Fe Kalpha line profile of the
Seyfert~1 galaxy MCG-06-30-15 is strongly variable. We attempt accretion disk
model fits to the Fa Kalpha line profiles in a high, low and medium continuum
luminosity phase of this source. During the monitoring by Iwasawa et al. (1996)
a broad red-shifted component remained reasonably constant while a narrower
component at $\approx$ 6.4 keV strongly responded to continuum changes.
Physically consistent fits are possible if the index xi of the power-law
emissivity changes from 0.7 (high phase) to 3.0 (low phase).
  The shape of the red-shifted component at low phase is crucial to the disk
model interpretation. We suggest that the actual shape may be a broad
redshifted Gaussian. Three lines of evidence support the interpretation of the
Fe Kalpha line as multicomponent, beyond the lack of correlation in the
response to continuum changes of the red and blue components in MCG -06-30-15.
(1) We show that the strong concentration of narrow peak centroids at 6.4 keV
is inconsistent with expectations of a random distribution of disk
orientations. (2) The average Fe Kalpha profile for a sample of 16 mostly
Seyfert~1's suggests a natural decomposition into two Gaussians one
unshifted/narrow and the other redshifted/broad. (3) Evidence for emission in
excess to the expectation of disk models on the high energy side of the Fe
Kalpha profile is both a challenge for low inclination disk models and support
for the two component decomposition.
