  We present the first results of a spectroscopic study of young massive stars
in the SMC High Excitation Blob N81. These stars have Mv values which are ~ 2
mag smaller than those of nor mal dwarf stars. Their UV STIS spectra reveal
features typical of O stars, but surprisingly weak wind components. The
preliminary modelling of these spectr a with the code CMFGEN (Hillier & Miller
1998) indicates a mass loss rate of the order 10e-9 Mdot/yr. 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.
