The detection of wind variability in Magellanic Cloud O stars

We present Far Ultraviolet Spectroscopic Explorer (FUSE) spectra for three Magellanic Cloud O stars (Sk 80, Sk -67 degrees 05, and Sk -67 degrees 111) with repeated observations. The data demonstrate the capabilities of FUSE to perform time-resolved spectroscopy on extragalactic stars. The wavelengt h coverage of FUSE provides access to resonance lines due to less abundant species, such as sulfur, which are unsaturated in O supergiants. This allow s us to examine wind variability at all velocities in resonance lines for s tars with higher mass-loss rates than can be studied at longer (lambda grea ter than or equal to 1150 Angstrom) wavelengths. The FUSE wavelength range also includes resonance lines from ions that bracket the expected dominant ionization stage of the wind. Our observations span 1-4 months with several densely sampled intervals of 10 hr or more. These observations reveal wind variability in all of the program stars and distinctive differences in the ionization structure and timescales of the variability. Sk -67 degrees 111 demonstrates significant wind variability on a timescale less than 10 hr, and the coolest O star (Sk -67 degrees 05) exhibits the largest variations in O VI.