The SW Sextantis stars are a group of cataclysmic variables with distinctive observational characteristics, including absorption features in the emission-line cores at phases 0.2-0.6. Hellier & Robinson have proposed that these features are caused by the accretion stream flowing over the accretion disk. However, in a simple model the absorption occurred at all orbital phases, which is contradicted by the data. I show that invoking a flared accretion disk resolves this problem.
Publications of the Astronomical Society of the Pacific
- Pub Date:
- April 1998
- STARS: EMISSION-LINE;
- ACCRETION DISKS;
- 4 pages, 3 figures, LaTeX, To appear in PASP. Also at http://www.astro.keele.ac.uk/~ch/