Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-25T14:29:24.485Z Has data issue: false hasContentIssue false

The Accretion Disk in DQ Her

Published online by Cambridge University Press:  12 April 2016

J. A. Petterson*
Affiliation:
Department of Physics, University of Illinois at Urbana-Champaign

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

DQ Her is one of the best studied Cataclysmic Variables. It is a classical nova which erupted in 1934 (Nova Herculis). Its optical lightcurve does not repeat accurately from one binary cycle to the next, but usually looks roughly like it does in Fig. 1. The small hump and small eclipse-asymmetry are probably both caused by the hot spot at the outer rim of the disk. The eclipse depth of ~90% argues for an inclination angle near 90°.

Type
Colloquium Session VI
Copyright
Copyright © The University of Rochester 1979

References

Alpar, M. A. 1979, preprint.Google Scholar
Chanan, G. A., Nelson, J. E., and Margon, B. 1978, Ap. J. 226, 963.Google Scholar
Chester, T. J. 1979, Ap. J. 230, 167.CrossRefGoogle Scholar
Herbst, W. Hesser, J. E., and Ostriker, J. P. 1974, Ap. J. 193, 679.Google Scholar
Kiplinger, A. L. and Nather, R. E. 1975, Nature 225, 125.Google Scholar
Papaloizou, J., and Pringle, J. E. 1977, M.N.R.A.S. 181, 441.Google Scholar
Patterson, J., Robinson, E. L., and Nather, R. E. 1978, Ap. J. 224, 270.Google Scholar
Petterson, J. A. 1979, preprint.Google Scholar
Rees, M. J. 1974, added note in M.N.R.A.S. 166, 113.Google Scholar
Shakura, N. I., and Sunyaev, R. A. 1973, Astron. and Astrophys. 24, 337.Google Scholar