Radiatively driven winds with azimuthal symmetry: application to Be stars

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Abstract
We present a radiatively driven wind model with azimuthal symmetry. Rotation effects and simulation of viscous forces were included in the motion equations. Distortion of the star as well as gravity darkening were also included in our computations. An application to Be stars leads to mass-flux ratios between equator and pole of the order of 10 and total mass-loss rates in the range 10−7 to 10−8 |$M_\odot\enspace \text {yr}^{-1}$|⁠. Our envelope models are flattened towards the equator and the wind terminal velocity in that region is comparable to the values attained in the polar direction.

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