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Nonlinear electromagnetic wave interactions in Hall–MHD plasmas

Published online by Cambridge University Press:  02 September 2010

DASTGEER SHAIKH  and
P. K. SHUKŁA
DASTGEER SHAIKH
Affiliation:
Department of Physics and Center for Space Physics and Aeronomic Research (CSPAR), University of Alabama at Huntsville, Huntsville, AL 35805, USA ([email protected])
P. K. SHUKŁA
Affiliation:
Institut für Theoretische Physik, Fakultät für Physik und Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany ([email protected])
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Abstract

We have developed a massively parallelized fully three-dimensional (3D) compressible Hall–magnetohydrodynamic (MHD) code to investigate inertial range electromagnetic wave cascades and dissipative processes in the regime, where characteristic length scales associated with plasma fluctuations are smaller than ion gyroradii. Such regime is ubiquitously present in the solar wind and many other collisionless space plasmas. Particularly, in the solar wind, the high time resolution databases depict a spectral break near the end of the 5/3 spectrum that corresponds to a high-frequency regime where the electromagnetic turbulent cascades cannot be explained by the usual MHD models. This refers to a second inertial range, where turbulent cascades follow a k−7/3 (where k is a wavenumber) spectrum in which the characteristic electromagnetic fluctuations evolve typically on kinetic Alfvén time scales. In this paper, we describe results from our 3D compressible Hall–MHD simulations that explain the observed k−7/3 spectrum in the solar wind plasma, energy cascade, anisotropy, and other spectral features.

Type
Papers
Information
Journal of Plasma Physics , Volume 76 , Special Issue 6: Advances in Photon Physics , December 2010 , pp. 893 - 901
Copyright
Copyright © Cambridge University Press 2010

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