Abstract
High-resolution short-wavelength IUE spectra were used to characterize the eclipsing binary system V444 Cygni. Light curves derived from the data revealed a 'third light' in the system that could not be modeled solely in terms of the eclipse of one limb-darkened disk by another. The UV-visible light curve corresponded with one O component (10 solar masses) at an effective temperature (Teff) of 40,000 K and a WR star (9 solar masses) with a Teff of 30,000 K. The WR star is projected to have large, readily visible, magnetic field-supported plumes enveloping both stars. Light scattering by electrons in the plumes would cause the anomalies observed in the emission-line spectrum and continuum light from the objects.
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