Abstract
The light curves of four close binary star systems (BV 267, RU UMi, XZ CMi, and VV UMa) have been analyzed using the Wilson-Devinney differential corrections model. The present system geometries of these binaries is that of short-period semi-detached systems with Roche-lobe-filling secondaries and main-sequence primaries. Differential coordinates in the mass-luminosity and mass-radius diagrams indicate that the secondary components lie near the main sequence, except in the case of BV 267. It is suggested that these systems are binaries with slightly overluminous and oversized secondaries which have undergone case A mass transfer. This contention is supported by timing information, and qualitatively by the period-frequency relation. These very-nearly contact binaries are likely candidates for postcontact system evolution. 34 refs.
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