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The classical T Tauri star GW Ori is found to be a spectroscopic binary whose orbital period is 242 days. Radial velocity data are presented which show that GW Ori is a velocity variable, the spectroscopic orbital elements are listed, and the dynamic masses for secondary and primary/secondary separations at different inclination angles are given. Two theoretical models for the spectral energy distribution are considered in detail, based on the binary's flux distribution which is double peaked with a strong silicate emission. The pure-disk model, consisting of a primary star, both a circumprimary and circumbinary disk, and optically thin hot dust between the disks, is found to fit the spectral distribution with the exception of higher luminosity in the 13-18 micron range. A disk-shell model is also considered in which an optically thin shell replaces the circumbinary disk. This model fits the spectral distribution well although the visual extinction must be larger than the observed A(v). The significance of the circular orbit theorized for the binary is considered with special attention given to the disk-induced excitation of eccentricity in binary orbits.
Mathieu et al. (Sat,) studied this question.