We model the line profile variability (lpv) in spectra of clumped stellar atmospheres using the
Stochastic Clump Model (SCM) of the winds of early-type stars. In this model the formation
of dense inhomogeneities (clumps) in the line driven winds is considered as being a stochastic
process. It is supposed that the emission due to clumps mainly contributes to the intensities of
emission lines in the stellar spectra. It is shown that in the framework of the SCM it is possible
to reproduce both the mean line profiles and a common pattern of the lpv.