FULL-ORBIT H-ALPHA EMISSION IN RW TAURI

Halpha observations of the Algol system RW Tauri were obtained over a four-year period (1988 October-1992 September) at approximately 1 angs trom resolution, with coverage over the full orbit. Strong single-peak ed emission near orbital quadrature is easily seen in the raw spectra. Subtracting the stellar components' light reveals a second, weaker, o ften double-peaked emission component at almost all phases, at most ep ochs. An absorption component is seen just before and after primary ec lipse. Visibility and velocities for the strong emission place it betw een the stellar components, near the primary star. Depending on the ep och, this stronger emission has one of two distinct patterns in a velo city versus phase plot. The weaker emission feature's visibility and v elocity indicate that it usually arises from a slowly rotating structu re near the primary star, with a radial extent of at least 0.33 R1. A third feature (which we interpret as a transient ring) was present in 3 of 12 runs.