Abstract
Based on 1-dimensional numerical simulations including the rotational acceleration in a quasi-spherical approximation we present pulsation-driven mass loss from luminous stars. In particular, for our model WN8 with M = 60 M ๏ , L = 8×10 5 L ๏ and T eff = 25 000 K with a rotation rate of v sin i = 160 km s -1 given at the stellar photosphere of R p = 47.6 R ๏ and a stellar pulsation of P = 4.144 days we compute a time-dependent mass loss with an averaged rate of 1.28×10 -4 M ๏ /yr. Further implications of such theoretical models are briefly discussed for observations of variable stars with large amplitudes.
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