Abstract. 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, a and S which control the dynamics of the flow. We apply our models to the problem of disk formation in B[e]-star winds. Winds from rotating early-type starsIn recent years, the actual structure of radiation driven winds from rotating early-type stars has been discussed without resolution. Bjorkman & Cassinelli (1993) dropped for the first time the assumption of spherical symmetry and solved for the particle trajectories in the polar plane, thus adopting only azimuthal symmetry about the rotational axis. In the equations of motion, they considered additionally to the inertial accelerations a purely radial line force calculated within the force-multiplier concept, where the corresponding forcemultiplier parameters (fmps) kcAK, <*, 5 (cf. Castor et al. 1975, Abbott 1982 were assumed to be constant throughout the wind, i.e., independent both of distance r and co-latitude 0 .This model predicts a polar deflection of the wind material towards the equatorial plane leading to the formation of a wind-compressed disk (WCD) in the equatorial plane for extreme rotation rates Q > 0.9(0.5) for 0-(B-)stars (for a confirmation by radiation hydrodynamical simulations, see Owocki et al. (1994). Owocki et al. (1996) additionally accounted for non-radial line force components <7Q nes and g$ nes (acting in the polar and azimuthal direction, respectively) and gravity darkening.The negative <7Q nes inhibits the disk formation and redistributes the wind material towards the poles, and the negative <7$ nes spins down the wind (by up to < 35% of the value given by angular momentum conservation). The gravity darkening implies an enhanced (reduced) photon flux over the poles (in the equatorial plane) and thus leads, in combination with the non-radial line force components, to an unambigously prolate wind, which is dense and fast over the poles and slower and thinner in the equatorial plane. These results are entirely contradictory to the predictions by the simple BC model and, meanwhile, have been independently confirmed by Petrenz (1999).However, also these investigations suffer from the assumption of fccAK, ct, 8 constant throughout the wind, which have been adopted from 1-D non-LTE 626 terms of use, available at https://www.cambridge.org/core/terms. https://doi
Abstract. The present state of modelling radiatively driven stellar winds from rapidly rotating stars is reviewed. Various processes a ecting the actual, still controversial wind structure are highlighted, in particular non-radial line-forces and gravity d a r k ening, and useful scaling relations are provided. The importance of accounting for consistentNLTE line-forces depending both on the actual density structure and radiation eld (as function of latitude and radius) is stressed, and some independent test calculations con rming earlier numerical results are reported.
Abstract. The present state of modelling radiatively driven stellar winds from rapidly rotating stars is reviewed. Various processes a ecting the actual, still controversial wind structure are highlighted, in particular non-radial line-forces and gravity d a r k ening, and useful scaling relations are provided. The importance of accounting for consistentNLTE line-forces depending both on the actual density structure and radiation eld (as function of latitude and radius) is stressed, and some independent test calculations con rming earlier numerical results are reported.
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