Abstract
The eclipsing binary WY Cancri (G5 V, M2 V), having a period of od. 82937122, has been classified as a short period RS CVn type binary (Hall, 1976). Chambliss (1965), Oliver (1976, Sarma (1976), Awadulla and Budding (1979) have reported observations of this system. In order to determine a more reliable period of the distortion wave, its source, nature and period of the overall luminosity change from one observing season to the next, we have included this star in the observing schedule of RS CVn binaries at our observatory. Observations were made in standard UBV filters using the ^48-inch reflector telescope of the Japal-Rangapur Observatory. The stars BD+28° 1672 and BD+27° 1701 were used as a comparison and check stars respectively.
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