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Deutsche Physikalische Gessellschaft IOP Institute of Physics

A model of nonlinear evolution and saturation of the turbulent MHD dynamo

Focus on Turbulence in Magnetized Plasmas

A A Schekochihin1, S C Cowley1, G W Hammett1,3, J L Maron1,4 and J C McWilliams2

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Part of Focus on Turbulence in Magnetized Plasmas

The growth and saturation of magnetic field in conducting turbulent media with large magnetic Prandtl numbers are investigated. This regime is very common in low-density hot astrophysical plasmas. During the early (kinematic) stage, weak magnetic fluctuations grow exponentially and concentrate at the resistive scale, which lies far below the hydrodynamic viscous scale. The evolution becomes nonlinear when the magnetic energy is comparable to the kinetic energy of the viscous-scale eddies. A physical picture of the ensuing nonlinear evolution of the MHD dynamo is proposed. Phenomenological considerations are supplemented with a simple Fokker-Planck model of the nonlinear evolution of the magnetic-energy spectrum. It is found that, while the shift of the bulk of the magnetic energy from the subviscous scales to the velocity scales may be possible, it occurs very slowly - at the resistive, rather than dynamical, timescale (for galaxies, this means that the generation of large-scale magnetic fields cannot be explained by this mechanism). The role of Alfvénic motions and the implications for the fully developed isotropic MHD turbulence are discussed.


PACS

52.35.Ra Plasma turbulence

52.35.Mw Nonlinear phenomena: waves, wave propagation, and other interactions (including parametric effects, mode coupling, ponderomotive effects, etc.)

47.65.-d Magnetohydrodynamics and electrohydrodynamics

52.65.Ff Fokker-Planck and Vlasov equation

52.30.Cv Magnetohydrodynamics (including electron magnetohydrodynamics)

Subjects

Fluid dynamics

Plasma physics

Dates

Issue 1 (October 2002)

Received 24 July 2002, in final form 26 September 2002

Published 30 October 2002



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