ECLIPSES IN CATACLYSMIC VARIABLES WITH STATIONARY ACCRETION DISKS .2.UX UMA

It is proposed to divide the light curves of UX UMa, according to thei r shapes, into two types: (1) The standard light curves, showing a wel l defined orbital hump, due to the hot spot, which occurs in the phase interval from about phi = -0.4 to about phi = 0.1, its declining part being still visible after the eclipse. (2) The peculiar light curves, showing either an ill defined orbital hump of a much smaller amplitud e, or even a depression in the phase interval, where the hump is norma lly present. Using a new approach, described in Paper I, the B and V l ight curves of UX UMa, observed between 1952 and 1961 by Johnson et al . (I 954), Walker and Herbig (1954), and Krzeminski and Walker (1963), were analyzed. The standard mean light curves of 1953 and 1955 were s uccessfully decomposed into their disk and spot components. From the a nalysis of the disk and spot eclipses the basic system parameters were then determined: M1 = (0.7 +/- 0.2) M., M2 = (0.48 + 0.02) M., A = (1 .05 +/- 0.08) x 10(11) cm, i = 73.0 +/- 1.8, R(d)/A = 0.34 +/- 0.03, M = (6.6 +/- 2.2) x 10(17) g/s, and the distance d=328 +/- 12 pc. The v alue of K1 = 150 +/- 18 km/s, predicted from these parameters, is in p erfect agreement with spectroscopic determinations. The standardlight curves of March 1952, which were brighter by 0.14 - 0.18 mag, were ana lyzed in the same way giving: M almost-equal-to 8 x 10(17) g/s and R(d )/A almost-equal-to 0.38. The analysis of the peculiar mean V light cu rves of 1958 and 1961, and UBV light curves of 1952 May 29 revealed th at their peculiarities are due to absorption produced by ''circumdisk' ' material. Consequently, the peculiar light curves cannot be used in the analysis of the disk or spot eclipses.