The recent Voyager encounter with Uranus has produced new insights and observational constraints on the structure, composition, and evolution of the Uranian rings. We have made careful measurements of the brightness variation as a function of longitude for the &agr;, &bgr;, &ggr;, Δ, and ϵ rings. The measurements showed a substantial variation in azimuthal brightness because of the varying width of the rings. The single scattering albedo of the ϵ ring particles was found to be 3.9%¿0.6% (for the Lambert surface) or 2.3%¿0.4% assuming the ''lunar-type'' phase function. The optical depth at apoapse of the ϵ ring was found to be 0.40¿0.05. Note that this determination of the optical depth is independent of the occultation measurement from Earth or from the spacecraft. This value is the optical depth for reflected light, whereas occultation data provide the forward scattering optical depth. It is consistent with varying amounts of mutual shadowing of ring particles due to changing width of the ring along its orbit. The single scattering albedo of the &agr;, &bgr;, &ggr;, and Δ rings is consistent with the ϵ ring, however, with bigger error bars (between 1.5 and 2.0%¿0.5% assuming the ''lunar-type'' phase function). ¿ American Geophysical Union 1987