Accretion disc viscosity - A simple model for a magnetic dynamo

Details Accretion disc viscosity - A simple model for a magnetic dynamo Accretion disc viscosity - A simple model for a magnetic dynamo

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.259..604t&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 259, no. 4, p. 604-612.

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135

Accretion Disks, Astronomical Models, Dynamo Theory, Magnetic Field Reconnection, Computational Astrophysics, Equilibrium Equations, Viscosity

Scientific paper

We develop here a simple physical model for the manner in which a magnetic dynamo might operate in an accretion disk and so provide an effective (magnetic) viscosity. In contrast to other dynamo models, the mechanism we discuss does not depend on the existence of some hydrodynamical small-scale turbulent flow hypothesized to be already present in a nonmagnetic disk. Rather, the model we present depends on three well-established physical processes: the Parker instability, the Balbus-Hawley instability and magnetic field reconnection. The model gives rise to finite but nonstationary magnetic field configurations. For the set of parameters chosen here we find a time-averaged effective viscosity with Shakura-Synyaev alpha-parameter around alpha(SS) of about 0.4.

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