An analysis of seven A-type W UMa eclipsing binary stars (V566 Oph, RR Cen, FG Hya, DK Cyg, BU Vel, UZ Leo and ϵ CrA) using the Wilson–Devinney computer code is presented. The main goals were (a) determining accurate values of the bolometric albedo, gravity darkening exponent, and linear limb darkening coefficients for these systems, and (b) analysing light curves from several different epochs in order to detect system parameter changes in V566 Oph, RR Cen and UZ Leo. The results show that a gravity darkening exponent g = 0.2 is preferred by the systems in this sample, the linear limb darkening coefficients show systematic deviations from the theoretical values predicted by currently accepted stellar atmosphere models, and a wide range of values of the bolometric albedo, A, is indicated. Reanalysis of FG Hya and DK Cyg removes the problem of fitting primary eclipse for these systems found by Mochnacki & Doughty (1972).
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Laurence Twigg (1979) studied this question.