Abstract
Rotationally-distorted radiative wind models driven by optically thin lines are examined. The basic equations are presented and some particular cases are applied to B[e] supergiant equatorial disks. We have taken into account a viscosity parameter, which simulates viscous effects in the rotational law, and we considered some ad-hoc temperature profiles. Observational expansion velocities (Vexp ≈ 100 km s-1) may be reproduced if: (i) the number of driving lines is near the maximum admitted from physical considerations, or, (ii) there is a temperature increase throughout the envelope. These situations are discussed. We suggest that thin line radiative forces may play a significant role in the dynamics of B[e] excretion disks.
