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Session 43 - Binary Stars.
Display session, Tuesday, January 16
North Banquet Hall, Convention Center
AX Monocerotis is unusual for a binary with an \approx 232^d.5 orbital period: a K giant star, a Be-like giant star, and large amounts of circumbinary material. Either or both components may be in contact with their critical lobes. The Be star exhibits very wide line widths corresponding to v\sini \sim 230 km s^-1, which may or may not be related to the stellar rotation rate. We present several possible models for AX Mon based on 1) archival visible photometry, 2) archival ultraviolet spectroscopy, 3) new and archival visible spectroscopy, 4) new visible polarimetry, and 5) new radio photometry. Additional comments are presented concerning how optical interferometer observations would improve the orbital elements (resolving the stars in continuum) and provide additional information concerning its circumbinary environment (resolving the envelope in hydrogen emission, Mg II absorption, and Na I absorption).
