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The timescales and heating efficiency of MHD wave‐driven turbulence in an open magnetic region;



Incompressible MHD waves propagating in a non‐homogeneous background, with Alfven speed parallel gradients, can interact with their reflections producing a strong turbulent energy cascade to small perpendicular length scales. In an open magnetic region, with a strong background magnetic field, this nonlinear process can be described by the reduced MHD equations, in which incompressible or weakly compressible fluctuations are transverse to the mean field and their gradients in the parallel direction are much weaker than in the perpendicular direction. The system is forced by Alfven waves injected through the bottom boundary, with characteristic perpendicular length scale, amplitude and frequency. We identify the relevant timescales of the system and propose an ordering which favors the turbulent dissipation efficiency. We have applied this mechanism for the heating of the lower corona required in models of the origin of the solar wind. © 2003 American Institute of Physics;



AIP Conference ProceedingsAmerican Institute of Physics

Published: Sep 2, 2003

Keywords: solar wind; solar corona; plasma magnetohydrodynamics; interplanetary magnetic fields; plasma heating; plasma turbulence

DOI: 10.1063/1.1618610

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