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Magnetohydrodynamic Turbulence in Accretion Discs: Towards More Realistic Models

Published online by Cambridge University Press:  12 April 2016

Ulf Torkelsson ,
Axel Brandenburg ,
Åke Nordlund  and
Robert F. Stein
Ulf Torkelsson
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 9JN, United Kingdom
Axel Brandenburg
Affiliation:
Department of Mathematics, University of Newcastle upon Tyne, NE1 7RU, United Kingdom
Åke Nordlund
Affiliation:
Theoretical Astrophysics Center, Juliane Maries vej 30, DK–2100 Copenhagen, Ø, Denmark
Robert F. Stein
Affiliation:
Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA

Abstract

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The shearing box has rapidly become the accepted way to investigate turbulence in Keplerian shear flows. In this paper we discuss to what extent and in which way the outcome of the shearing box is affected by the adopted boundary conditions, and how the shearing box can be modified to capture more of the physics of an accretion disc. The original shearing box model is too symmetric to generate a net accretion flow, but the symmetry can be broken by including the main effects of the cylindrical geometry of the real disc. However the quantitative change in the resulting angular momentum transport is small.

Keywords

accretionaccretion discs – MHD – turbulence – magnetic fields
Type
Part 5. Magnetic Fields and Viscosity
Information
International Astronomical Union Colloquium , Volume 163: Accretion Phenomena and Related Outflows , 1997 , pp. 210 - 214
Copyright
Copyright © Astronomical Society of the Pacific 1997

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