Abstract
Charge-coupled device photometric observations of the W UMa-type binary star UX Eridani are presented. Comparing the B light curve with that obtained by Binnendijk in 1964-1965, the variation of the light curve around the primary minimum was found. Photometric solutions of Binnendijk's and our light curves were derived by using the new version of the Wilson-Devinney program. Our solutions confirmed that UX Eri is a marginal W-type overcontact binary system with a very low degree of overcontact, f 44.5 circle dot. The tertiary component may have played an important role in the formation of the progenitor of UX Eri by transferring angular momentum during the Kozai oscillation. In that way, the detached progenitor could evolve into overcontact configuration via magnetic braking. It was found that the timescale of the period increase is close to the thermal timescale of the less massive component, which suggests that UX Eri is in an evolutionary state of thermally conservative mass transfer from the less massive component to the more massive one.
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