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A PHOTOMETRIC STUDY OF THE ECLIPSING BINARY STAR SYSTEM RU URSAE MINORIS

The absolute elements of the close eclipsing system RU Ursae Minoris have been determined, using only photometric data. The calculation is based on an eclipsing binary computer model and on the following assumptions: 1. Relationship between stellar mass and distortion as determined by Chandrasekhar. 2. Applicability of the Stefan and Planck laws. 3. Applicability of the main-sequence mass-luminosity law to the primary star. Both stars are apparently oversize for their masses and temperatures. The FO dwarf primary star fills its Roche limiting surface. The secondary star contributes only about 3 percent of the system's yellow light, and is likely a late K dwarf with a radius of nearly 90 percent of its Roche limit. The system appears to be much like a W Ursae Majoris system, but with an exceptionally cool, faint secondary. Key words: variable star - photometry