Using Wood's (1972) model, the photoelectric observations of de Santis and Tempesti (1977) - as y... more Using Wood's (1972) model, the photoelectric observations of de Santis and Tempesti (1977) - as yet only crudely studied - of the eclipsing binary RT UMi are reanalyzed. The photometric elements that are derived greatly differ from previous ones and permit a coherent (semi-detached) picture of this binary. The F 0 primary appears to be accompanied by a fainter and smaller (early K) cooler star, which fills its Roche lobe for the photometric mass ratio q = 0.3. The absolute elements of RT UMi, tentatively estimated by assuming for the primary a mass of 1.7 solar masses, reveal that the primary has probably slightly evolved from the main sequence, while the secondary (probably a subgiant) is clearly oversized and overluminous for its mass and temperature, as common post-mass-exchange subgiant secondaries of semi-detached systems.
Using Wood's (1972) model, the photoelectric observations of de Santis and Tempesti (1977) - as y... more Using Wood's (1972) model, the photoelectric observations of de Santis and Tempesti (1977) - as yet only crudely studied - of the eclipsing binary RT UMi are reanalyzed. The photometric elements that are derived greatly differ from previous ones and permit a coherent (semi-detached) picture of this binary. The F 0 primary appears to be accompanied by a fainter and smaller (early K) cooler star, which fills its Roche lobe for the photometric mass ratio q = 0.3. The absolute elements of RT UMi, tentatively estimated by assuming for the primary a mass of 1.7 solar masses, reveal that the primary has probably slightly evolved from the main sequence, while the secondary (probably a subgiant) is clearly oversized and overluminous for its mass and temperature, as common post-mass-exchange subgiant secondaries of semi-detached systems.
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