Published online by Cambridge University Press: 07 August 2017
There are many indications for the existence of dense cold clumps in Wolf-Rayet (WR) atmospheres, expanding outwards from the stellar core (e.g., Cherepaschuck et al. 1984, St-Louis et al. 1993). Based on this, we consider a clump model for WR model atmospheres. The main features of the model are described. The mechanism of clump structure formation is outlined. The clump model is used for calculating emission line profiles.