Résumé
We present the first results of a spectroscopic study of young massive stars in the SMC high excitation blob N 81. These stars have M v values which are ~ 2 mag smaller than those of normal dwarf stars. Their UV HST -stis spectra reveal features typical of O-type stars, but surprisingly weak wind components. The preliminary modeling of these spectra with the code cmfgen (Hillier & Miller 1998) indicates mass loss rates of the order of 10 –9 M ⊙ yr –1 . If confirmed, such a weak wind may indicate either a breakdown of the wind-momentum luminosity relation at low luminosity, or a steeper slope of this relation at low metallicity.