3-D RADIATIVE LINE TRANSFER FOR BE STAR ENVELOPES

Based on numerical three-dimensional radiative line transfer calculati ons Halpha emission line profiles of circumstellar Be star envelopes h ave been derived. The results show that the so-called winebottle-type emission line profiles can be explained by the combination of rotation al broadening and non-coherent scattering in optically thick Keplerian disks. In a further calculation the stellar wind model of Be star env elopes has been re-investigated assuming an additional expansion compo nent in the velocity field. The resulting asymmetric winebottle-type p rofiles and asymmetric shell-type emission lines with blue-shifted cen tral depressions are in contradiction with the observed line shapes. I t is concluded that isotropic stationary outflows are not suitable to explain observed asymmetric emission line profiles of Be stars.