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MHD Turbulence in an Accretion Disk

Published online by Cambridge University Press:  25 April 2016

John F. Hawley  and
Steven A. Balbus
John F. Hawley
Affiliation:
University of Virginia, PO Box 3818, Charlottesville, VA 22903, USA. jh8h@virginia.edu, sb@virginia.edu
Steven A. Balbus
Affiliation:
University of Virginia, PO Box 3818, Charlottesville, VA 22903, USA. jh8h@virginia.edu, sb@virginia.edu
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Abstract

A long-standing problem in the theory of astrophysical accretion disks has been to determine the nature of the stress that transports orbital angular momentum outward. The discovery of a local MHD instability is strong evidence that transport occurs through turbulent Maxwell and Reynolds stresses. Using numerical simulations, we have demonstrated that a weak seed magnetic field in an accretion disk shear flow is unstable and leads to sustained MHD turbulence at dynamically important levels.

Keywords

accretionaccretion disksinstabilitiesMHD
Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 12 , Issue 2 , August 1995 , pp. 159 - 164
Copyright
Copyright © Astronomical Society of Australia 1995

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