Voyager 2 obtained images of Titania over phase angles ranging from 0.8¿ to 150¿ and at sufficient resolution to investigate the photometric behavior of different surface units. The large, relatively narrow opposition surge detected from Earth was confirmed and can be successfully modeled with Hapke's (1986) photometric theory. Opposition effects do not vary greatly between bright areas (craters and ejecta) and dark areas. The primary difference in phase behavior is that the brightness of the dark areas. Thus, contrary to the situation on the Moon the fresher craters and their ejecta become less prominent in relation to the background as opposition is approached. This effect is best explained by a modest difference in single-scattering albedo. There is evidence that the angular width of the opposition surge is slightly narrower for bright areas, a situation consistent with the interpretation that the ejecta regolith is somewhat less compacted than that in the background dark terrain. ¿ American Geophysical Union 1987