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Disk Emission Lines

Published online by Cambridge University Press:  12 April 2016

N. Murray  and
J. Chiang
N. Murray
Affiliation:
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ONT M5S 3H8, Canada
J. Chiang
Affiliation:
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ONT M5S 3H8, Canada

Abstract

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A thin disk illuminated by a central source will produce single-peaked broad emission lines if there is a wind emerging from the disk. The velocity gradient in the wind produces an anisotropic optical depth. For optically thick lines, the emission is strongest along directions perpendicular to the Keplerian velocity of the disk. The resulting line profiles are single peaked even though the emitting gas moves on essentially circular orbits. We argue that the broad emission lines seen in quasars, Seyferts, and luminous cataclysmic variables arise in disk winds.

Type
IV. Physics of the Broad-Line Region
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 220 - 221
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

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