Ha observations of the Algol system RW Tauri were obtained over a four-year period (1988 October-1992 at ~1 A resolution, with coverage over the full orbit. Strong single-peaked emission near orbital quadrature is easily seen in the raw spectra. Subtracting the stellar components' light reveals a second, weaker, often double-peaked emission component at almost all phases, at most epochs. An absorption component is seen just before and after primary eclipse. Visibility and velocities for the

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... ng emission place it between the stellar components, near the primary star. Depending on the epoch, this stronger emission has one of two distinct patterns in a velocity versus phase plot. The weaker emission feature's visibility and velocity indicate that it usually arises from a slowly rotating structure near the primary star, with a radial extent of at least 0.33 R x . A third feature (which we interpret as a transient ring) was present in 3 of 12 runs.