Balmer emission lines from cataclysmic variables often have nearly equal intensities rather than the rapid decrement predicted by simple nebular theory. Traditionally, this has been interpreted in terms of local thermodynamic equilibrium emission from a dense gas with small volume located just above the accretion disk. In this Letter we show that the intense radiation field within a close binary system can affect excited-state populations and optical emission in ways which allow a relatively low density gas to closely mimic the high-density situation. In at least one case, the old nova V603 Aql, the emitting gas has a low density and nearly fills the orbital plane of the system. If this is characteristic of other systems, then the determination of orbital parameters and masses of cataclysmic variables from emission-line radial velocities, as well as the prediction of soft X-ray emission from accreting binaries, will be affected.

Document Type


Publication Date


Notes/Citation Information

Published in The Astrophysical Journal Letters, v. 272, no. 2, p. L55-L59.

© 1983. The American Astronomical Society. All rights reserved.

The copyright holder has granted permission for posting the article here.

Digital Object Identifier (DOI)