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The Phase 0.5 Absorption in SW Sextantis–Type Cataclysmic Variables

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.