Conspicuous, variable photometric contamination was observed during primary eclipses of the totally eclipsing Algol-like system U Cep from late-1974 to late-1977. Excess light was particularly prominent between second and third contacts, and originated mainly in optically thick accretion disks surrounding the B-type hot component. Observations of such disks were obtained with uvby (I) photometry during 10 eclipses, using the 1.0 M and 0.4 M reflectors at Prairie and Kitt Peak National Observatories. Figure 1 shows ultraviolet observations between internal contacts for active (October, 1975) and quiescent eclipses. The light excess over quiescent levels was converted to flux distributions Lλc relative to the quiescent visual flux of. the G-star.