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Nonlinear Processes in Geophysics An interactive open-access journal of the European Geosciences Union
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Volume 12, issue 1
Nonlin. Processes Geophys., 12, 75–81, 2005
https://doi.org/10.5194/npg-12-75-2005
© Author(s) 2005. This work is licensed under
the Creative Commons Attribution-NonCommercial-ShareAlike 2.5 License.

Special issue: Advances in space environment turbulence

Nonlin. Processes Geophys., 12, 75–81, 2005
https://doi.org/10.5194/npg-12-75-2005
© Author(s) 2005. This work is licensed under
the Creative Commons Attribution-NonCommercial-ShareAlike 2.5 License.

  25 Jan 2005

25 Jan 2005

Modeling of short scale turbulence in the solar wind

V. Krishan1 and S. M. Mahajan2 V. Krishan and S. M. Mahajan
  • 1Indian Institute of Astrophysics, Bangalore 560 034, India
  • 2Institute for Fusion Studies, The University of Texas at Austin, Austin, Texas 78712, USA

Abstract. The solar wind serves as a laboratory for investigating magnetohydrodynamic turbulence under conditions irreproducible on the terra firma. Here we show that the frame work of Hall magnetohydrodynamics (HMHD), which can support three quadratic invariants and allows nonlinear states to depart fundamentally from the Alfvénic, is capable of reproducing in the inertial range the three branches of the observed solar wind magnetic fluctuation spectrum - the Kolmogorov branch f -5/3 steepening to f1 with $alpha_1{simeq}3{-}4$ on the high frequency side and flattening to f -1 on the low frequency side. These fluctuations are found to be associated with the nonlinear Hall-MHD Shear Alfvén waves. The spectrum of the concomitant whistler type fluctuations is very different from the observed one. Perhaps the relatively stronger damping of the whistler fluctuations may cause their unobservability. The issue of equipartition of energy through the so called Alfvén ratio acquires a new status through its dependence, now, on the spatial scale.

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