Abstract
ABSTRACT High-speed photometric UBV observations of the nova-like variable V Sagittae conducted during 1994 and 1995 are reported. The data consist of a total of 152 hours of observations, covering the entire 12.3 hr orbital period. Analysis of the photometry using the new Wilson eclipsing-binary code suggests a model where mass is being transferred from a 0.86 Msun, evolved, Helium-burning star, which fills its Roche lobe, to a 3.48 Msun evolved companion. Thirteen new timings of primary eclipse in conjunction with published timings from 1946 to 1996 show that the orbital period is changing at a rate dot {P} = -5.1(± 1.0) x 10-10 . We derive a lower limit to the mass loss rate from the primary star of dot {M1} ~ -4.4(± 0.1) x 10-7 Msun yr-1 . V Sge appears to be in a short-lived evolutionary state with a lifetime of ~ 2 x 106 yr.
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