The stochastic clump model of the winds of early-type stars based on the clump model of the wind is proposed. The formation of the inhomogeneities (clumps) in this model is considered as a stochastic process. The model is well suited both to obtain the mean line profile, which is very close to the observed one, and to reproduce an amplitude and a common pattern of the line profile variability in the spectra of the Wolf-Rayet and OB stars.