It is well known that the power stellar wind of OB and Wolf-Rayet (WR) stars consist of the numerous dense inhomogenuities (clumps) and more rarefied homogeneous interclump medium. Clumps are randomly distributed in the whole volume of stellar wind and have arbitrary sizes and fluxes. Formation of the clumps appears to be the chaotic process connected with internal instability of the radiation dominated stellar wind. Our modelling of the line profiles in spectra of OB and WR stars with clumped wind show that initially chaotic ensemble of the clumps can be regularized. As a result of that regularization the clusters of clumps which manifest themselves as strong bumps on the line profiles cam be developed.