Abstract
Empirical mass-loss rates of 28 luminous galactic OB stars are derived from thermal radio emission and from Hα recombination radiation. The velocity fields of all stars had previously been analyzed in the IUE ultraviolet spectral region. The results of these ultraviolet line-profile analyses (shape of the velocity law and terminal velocity) are combined with the radio and Hα data for a precise and consistent determination of the stellar mass-loss rates. It is found that radio and Hα rates agree within the observational errors. This suggests that significant clumping in the wind is unlikely due to the very different radius of origin of radio and Hα radiation within the wind
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