Ionization structure of the Wolf-Rayet stars of WC type has been investigated. The assumption that the atmospheres consists of H, He and C is made. The CIII lambda5696 line fluxes both for homogeneous atmosphere and for the atmosphere with the inhomogeneities inside it have been calculated. A dependence of the line profiles on the parameters of inhomogeinities is studied. The CIII lambda5696 line profiles calculated for an homogeneous atmosphere appeares to be too weak in comparison with the observed ones. To explain this discordance the supposition that a large ensemble of dense inhomogeneities presents in the atmosphere was made. The scaled relations connecting a mass of the inhomogeneity with the line flux in the profile bump, formed by it in the CIII lambda5696 line profile, are found. These relations are used to construct the stochastic model of the Wolf-Rayet star's atmospheres. The formation of the inhomogeneities in this model is considered to be a stochastic process. It is shown that the model is well suited to obtain the mean line profile, which is very close to the observed one, and to reproduce both an amplitude and a common pattern of the line profile variability in the spectra of the Wolf-Rayet stars. A wavelet anaysis method is used to find the relative contribution of the small and large sizes into the whole ensemble of the inhomogeinities.