Hostname: page-component-745bb68f8f-lrblm Total loading time: 0 Render date: 2025-01-27T11:22:03.936Z Has data issue: false hasContentIssue false
  • English
  • Français

Line Formation in U Gem and T Leo

Published online by Cambridge University Press:  12 April 2016

W. Hummel ,
K. Horne ,
T.R. Marsh  and
Janet H. Wood
W. Hummel
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Pleinlaan 2, B-1050 Brussel, Belgium
K. Horne
Affiliation:
University of St. Andrews, School of Physics & Astronomy, North Haugh, St. Andrews, Fife KY16 9SS, Scotland
T.R. Marsh
Affiliation:
University of Southampton, Department of Physics, Highfield, Southampton SO17 1BJ, England
Janet H. Wood
Affiliation:
Keele University, Department of Physics, Keele ST5 5BG, England

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.

We present 3-D LTE radiative transfer calculations [1] for H, He and Ca in accretion disks (AD) of dwarf novae in quiescence. The model disk is assumed to be in hydrostatic equilibrium vertically, and to rotate with Keplerian velocities. Calculated emission lines are fitted to phase-averaged, continuum-subtracted spectra of U Gem (Fig. 1) and T Leo (Fig. 2). Up to four parameters of the AD have been fitted: distance D, baryonic number density N, isotropic turbulence Vtu and disk temperature T; the latter two are assumed to be constant throughout the disk. Geometrical parameters are from [2] and [3].

Type
Non-Magnetic Cataclysmic Variables
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 87 - 88
Copyright
Copyright © Kluwer 1996

References

1. Hummel, W., 1994, A&A, 289, 458 Google Scholar
2. Marsh, T.R., Horne, K., Schlegel, E.M., et al., 1990, Ap. J., 364, 637 Google Scholar
3. Shatter, A.W., Szkody, P., 1984, Ap. J., 276, 305 Google Scholar