Radiation driven winds of hot luminous stars. II. Wind models for O-stars in the Magellanic clouds.

Wind models are calculated for O-stars in the Magellanic Clouds using the modified radiation driven wind theory developed by Pauldrach et al. (1986). For the calculation of the radiative line forces a lower metallicity is adopted: Z_LMC = 0.28×Z_GALAXY; Z_SMC = 0.1×Z_GALAXY. As a result, significantly weaker winds are obtained in the Clouds than in the Galaxy, which show smaller mass-loss rates Mand terminal velocities v. The calculations, in which wind models computed along evolutionary tracks for each of the three galaxies are used, confirm quantitatively the observations of Garmany and Conti (1985) who found generally lower terminal velocities in the Clouds.