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Dynamo Driven Accretion Discs and Dwarf Nova Eruptions

Published online by Cambridge University Press:  12 April 2016

P.J. Armitage ,
M. Livio  and
J.E. Pringle
P.J. Armitage
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, CB3 OHA, UK
M. Livio
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
J.E. Pringle
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, CB3 OHA, UK Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

Extract

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A magnetic dynamo whose crucial ingredient is the Balbus-Hawley instability (Balbus & Hawley 1991) is a promising candidate for generating accretion disc viscosity. Both semi-quantitative analyses (Tout & Pringle 1992) and simulations (e.g. Brandenberg et al. 1995) suggest that such dynamos can operate in a disc environment. Here we aim to apply simple dynamo ideas to models of dwarf novae, and in particular investigate how dynamo driven discs can produce different values for α in quiescence and in outburst.

Type
Accretion Discs
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 107 - 108
Copyright
Copyright © Kluwer 1996

References

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