Accretion disk evolution

Details Accretion disk evolution Accretion disk evolution

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.130..293b&link_type=abstract

(IAU, DFG, and Bayerisches Staatsministerium für Unterricht und Kultus, Colloquium on Cataclysmic Variables, Recent Multi-Freque

Astronomy and Astrophysics

Astrophysics

2

Accretion Disks, Dwarf Novae, Mass Transfer, Stellar Mass Ejection, Stellar Models, Systems Stability, Light Curve, Roche Limit

Scientific paper

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 is 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.

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