The stellar winds of early-type stars in the Small Magellanic Cloud.

Abstract

Low-resolution IUE spectra are used to investigate stellar winds of early-type stars in the Small Magellanic Cloud (SMC). Model profiles are used to fit well developed P Cygni doublets noted in 25 main-sequence, giant, and supergiant stars. Terminal velocities in the SMC are found to be, generally, up to a factor of 2 lower relative to galactic O stars of similar luminosity, reaching differences of about 1000 km/s. Although a reduction by a factor of about 3 is noted in the SMC C IV wind column densities, the products of mass loss rate and ion fraction are not seen to differ significantly from those of corresponding galactic O stars. The present results may suggest SMC mass loss rates which are similar to those observed in galactic stars of similar luminosity.