  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.
