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Recent results from simulations of the magnetorotational instability

Published online by Cambridge University Press:  08 June 2011

James M. Stone
James M. Stone*
Affiliation:
Department of Astrophysical Sciences, Princeton University, Princeton NJ 08540, USA, email: jmstone@princeton.edu
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Abstract

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The nonlinear saturation of the magnetorotational instability (MRI) is best studied through numerical MHD simulations. Recent results of simulations that adopt the local shearing box approximation, and fully global models that follow the entire disk, are described. Outstanding issues remain, such as a first-principles understanding of the dynamo processes that control saturation with no net magnetic flux. Important directions for future work include a better understanding of basic plasma processes, such as reconnection, dissipation, and particle acceleration, in the MHD turbulence driven by the MRI.

Keywords

accretion disksinstabilitiesMHDplasmasturbulencemethods:numerical

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 422 - 428
Copyright
Copyright © International Astronomical Union 2011

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