  Analyzing the archival data from the Rossi X-ray Timing Explorer (RXTE), we
study the power density spectra (PDS) of Cygnus X-1 from 1996 to 2003 in the
frequency range of 0.01 - 25 Hz. With our model we are able to track the
evolution of the Lorentzian components through all spectral states of the
source. We confirm the relation between characteristic frequencies seen both in
black hole candidate and neutron star sources, and show the changes in this
relation during the transitional and soft states of the source. The connection
between the Lorentzian components is investigated by analyzing similarities and
differences in their behavior. We find that the spectral state of the source
can be uniquely determined from the parameters of the these components. The
parameter correlations can all be described by continuous functions, which
differ between components. We discuss our results in the context of
relativistic precession model for the accretion disk, and show a remarkable
agreement between the model prediction and the data in the hard state. We
estimate a value for the specific angular momentum of a=+0.49 (-0.57) in the
case of prograde retrograde) rotation and an estimate for the inner radius of
22 to 50 (25 to 55) gravitational radii.
