Abstract
In order to quantify the effect of metallicity on the wind of massive stars, we determined mass-loss rates and terminal velocities for a sample of 29 LMC and SMC O stars and compared those values with results from Galactic stars. The author derived the desired quantities from HST UV spectra, optical spectra obtained at the CASLEO observatory and model atmospheres. She used the Schmutz (1998) code, which reproduces the hydrogen and helium lines present in the optical region, to determine the mass-loss rate, luminosity and temperature of each of the stars. Terminal velocities have been calculated with the SEI code. Radiation-driven wind theory predicts a strong dependence of the mass-loss rate with metallicity. Based on the observations, this dependence is not that strong, especially for giant and supergiant O stars. The author also finds that the terminal velocities of evolved O stars are almost insensitive to metallicity.
