Normalized flux distributions were measured for U Ophiuchi, AG Persei, lambda Tauri, and V356 Sagitarii from 1976 July to 1978 March. The spectra of lambda Tauri match those of a B4 star and an A4 star at phases 0.77--9.90, and those of a B3 star and an A4 star at other phases. The spectra of V356 Sagittarri match those of a B3 star and an AO star; however, the spectra at isolated phases show the excess ultraviolet light characteristics of hydrogen free-bound emission. The solutions for the system parameters given by Koch and Koegler and by Popper were found to satisfy the observed light curves for U Ophiuchi and AG Persei, respectively. Spectral evidence of circumstellar matter is not found for U Ophiuchi or AG Persei. The observed normalized flux distributions were compared to normalized flux distributions calculated as a function of phase from a computer model. It was not possible to separate the effects of limb darkening and temperature. For U Ophiuchi the following values are derived: E (B-V) =0.15 +- 0.03 mag, T/sub eff/=18,500 +- 1000 K and 17,400 +- 1100 K, M/sub upsilon/=-0.92 +- 0.50 mag and -0.93 +- 0.50 mag, and r=275 +- 80 pc. Itmore » the more massive star is the larger star, the values of M/sub upsilon/ are -1.05 and -0.80 mag. For AG Persei the values found are E (B-V) =0.24 +- 0.03 mag, T/sub eff/ =21,500 +- 1000 K and 19,500 +- 1100 K, M/sub upsilon/=-1.10 +- 0.50 mag and -0.60 +- 0.50 mag, and r=300 +- 80 pc.« less