The phase 0.5 absorption in SW Sextantis-type cataclysmic variables

Preprint

3 February 1998

preprint
Published by arXiv in arXiv

https://doi.org/10.48550/arXiv.astro-ph/9802042

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.

Keywords

CATACLYSMIC VARIABLES
TYPE CATACLYSMIC
SEXTANTIS TYPE
ACCRETION DISK
SW SEXTANTIS
ABSORPTION
FLARED

All Related Versions

Version 1, 1998-02-03, ArXiv
Published version: Publications of the Astronomical Society of the Pacific, 110 (746), 420.

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