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The BVR CCD observations of W UMa-type eclipsing binary SS Arietis were made for ten nights from November 1996 to December 1996 at the Sobaeksan Astronomy Observatory. From the observed light curves, nine new times of minimum lights were derived from the Kwee and van Woerden’s method. Improved light elements for this system were determined from these minimum lights with all the published minima. The analysis of the times of minima of SS Ari confirms that the orbital period of SS Ari has been suffering from a sinusoidal variation as the suggestions of other previous investigators (Kaluzny & Pojmanski 1984, Demircan & Selam 1993). The calculation shows that the cyclic period change has a period of about 56.3yrs with an amplitude of about 0.d052. The period variation has been discussed in terms of two potential mechanisms: 1) the light-time effect due to a hypothetical third body and 2) deformations in the convective envelope of a magnetically active component. The BVR light curves of SS Ari observed for about one month showed the existence of cycle to cycle light variations. Long-term light changes of SS Ari are discussed in terms of the period variation of the binary system.
Four times of minimum lights from six nights photoelectric observations of YY Eri during the observing seasons from 1983 to 1984 are derived. With these and previously published photoelectric minima, new light elements are determined. A detailed numerical investigation of times of minima shows that the orbital period has changed sinusoidally with a period of about 24 years. These changes of period are investigated in terms of two plausible causes : a light-time effect due to an unseen third body and asymmetries of light curves due to stellar activities of one component or both.
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