1999PASP..111..829S

A single-epoch low-resolution Goddard High Resolution Spectrograph spectrum of the eclipsing binary ε Aurigae was obtained while the secondary was orbiting toward eclipse by the primary. The spectrum as recorded between 1175 and 1461 Å is rich with emission and absorption lines which include stellar and interstellar components. The emission-line profiles have the appearance of double-peaked emission with a stronger red component at a radial velocity of +108 km.s^–1, an overlying unresolved absorption component at -20 km.s^–1, and a weaker blue emission bump at ~-92 km.s^–1. We compare these observational results with known orbital properties of the ε Aur binary system and propose that the emission originates at the inner radius of the disk surrounding the enigmatic secondary. We interpret the kinematic data as a possible means to uncover the underlying stellar masses, and we speculate about the binary's relationship to other ``high-mass'' models.