The Eclipsing Binary BG Geminorum: Improved Constraints on the Orbit and the Structure of the Accretion Disk

We describe new optical photometric and spectroscopic observations of the semidetached eclipsing binary BG Geminorum. A large change in the amount of Mg I absorption at secondary maximum indicates the presence of cool material in the outer edge of the disk surrounding the unseen primary star. Detection of weak He I emission implies a hot radiation source at the inner edge of the disk. If the velocity variations in the Hβ emission line track the orbital motion of the primary star, the primary star has an orbital semiamplitude of K1 = KHβ = 16.0 ± 4.6 km s . This result yields a mass ratio, q = 0.22 ± 0.07, consistent with the q = 0.1 derived from the large ellipsoidal variation. Despite this progress, the nature of the primary star – B-type star or black hole – remains uncertain. Subject headings: binaries: eclipsing – binaries: spectroscopic – stars: emission-line – stars: evolution – stars: individual (BG Gem)