The phase 0.5 absorption in SW Sextantis-type cataclysmic variables

Abstract

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 and 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.

4 pages, 3 figures, LaTeX, To appear in PASP. Also at http://www.astro.keele.ac.uk/~ch/

References in corpus (2)

• Hydrodynamics of the stream-disk impact in interacting binaries
• On the nature of SW Sex

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• SW Sextantis in an excited, low state
• The SW Sextantis stars
• Spectroscopy and orbital periods of four cataclysmic variable stars
• RX J1643.7+3402 : a new bright cataclysmic variable
• Photometry of the SW Sex-type nova-like BH Lyncis in high state
• Stream-field interactions in the magnetic accretor AO Piscium