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Accretion Disk Evolution

Published online by Cambridge University Press:  12 April 2016

G.T. Bath
G.T. Bath*
Affiliation:
Department of Astrophysics, Oxford, U.K.

Abstract

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Three aspects of mass transfer instability models of dwarf novae are examined. The hydrodynamic development of instabilities in the secondary are examined within Roche geometry and shown to extend at least a few degrees away from the line of centres. The form of the outburst light curves observed in SS Cygni are shown to be a natural consequence of mass transfer bursts with a duration either less than, or greater than, the disk viscous timescale. Finally the two-dimensional structure of the disc in the plane of the orbit is studied. As with α-disks the viscous evolution time following a burst of mass transfer determines the size of viscosity within the disk. Significant deviations from axial symmetry are found to be present.

Type
IV. Accretion Disks
Information
International Astronomical Union Colloquium , Volume 93: Cataclysmic Variables: Recent Multi-Frequency Observations and Theoretical Developments , 1987 , pp. 293 - 302
Copyright
Copyright © Reidel 1987

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