  We present model light curves for accreting Black Hole Candidates (BHC) based
on a recently proposed model for their spectro-temporal properties. According
to this model, the observed light curves and aperiodic variability of BHC are
due to a series of soft photon injections at random (Poisson) intervals near
the compact object and their reprocessing into hard radiation in an extended
but non-uniform hot plasma corona surrounding the compact object. We argue that
the majority of the timing characteristics of these light curves are due to the
stochastic nature of the Comptonization process in the extended corona, whose
properties, most notably its radial density dependence, are imprinted in them.
We compute the corresponding Power Spectral Densities (PSD), autocorrelation
functions, time skewness of the light curves and time lags between the light
curves of the sources at different photon energies and compare our results to
observation. Our model light curves compare well with observations, providing
good fits to their overall morphology, as manifest by the autocorrelation and
skewness functions. The lags and PSDs of the model light curves are also in
good agreement with those observed (the model can even accommodate the presence
of QPOs). Finally, while most of the variability power resides at time scales
$\gsim$ a few seconds, at the same time, the model allows also for shots of a
few msec in duration, in accordance with observation. We suggest that
refinements of this type of model along with spectral and phase lag information
can be used to probe the structure of this class of high energy sources.
