Selfconsistent models of winds from rotating early-type stars - Application to B[e] star winds

We present results of 2.5-D radiation hydrodynamical simulations of winds from rapidly rotating stars. For the first time, we consider the dependence of the line statistics on local density and radiation temperature implying a spatial variation of the force-multiplier parameters k, alpha and delta which control the dynamics of the flow. We apply our models to the problem of disk formation in B[e]-star winds.