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We study the effects of optically thick clumps, non-void inter-clump medium,variation of the onset of clumping, and velocity dispersion inside clumps onthe formation of resonance lines. For this purpose we developed a full 3-DMonte Carlo Radiative Transfer (MCRT) code that is able to handle 3-D shapes ofclumps and arbitrary 3-D velocity fields. The method we developed allows us totake into account contributions from density and velocity wind inhomogeneitiesto the total opacity very precisely. The first comparison with observationshows that 3-D density and velocity wind inhomogeneities have a very stronginfluence on the resonance line formation, and that they have to be accountedfor in order to obtain reliable mass-loss rate determinations.

3-D Monte Carlo radiative transfer calculation of resonance line formation in the inhomogeneous expanding stellar wind