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We discuss the development of the new radiative transfer code Wind3D. Itsolves the non-LTE radiative transport problem in moving stellar atmospheremodels in three geometric dimensions. The code accepts arbitrary 3D velocityfields in Cartesian geometry without assumptions of axial symmetry. Wind3D iscurrently implemented as a fully parallelized (exact) accelerated lambdaiteration scheme with a two level atom formulation. The numerical transferscheme is efficient and very accurate to trace small variations of localvelocity gradients on line opacity in strongly scattering dominated extendedstellar winds. We investigate the detailed formation of P Cygni line profilesobserved in ultraviolet spectra of massive stars. We compute the detailed shapeof these resonance lines to model local enhancements of line opacity that canfor instance be caused by clumping in supersonically expanding winds. Wind3Dwill be applied to hydrodynamic models to investigate physical properties ofdiscrete absorption line components.

Three Dimensional Radiative Transfer in Winds of Massive Stars: Wind3D