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Evolution of Alfvénic wave envelopes in spin-1/2 quantum Hall-magnetohydrodynamic plasmas

Phys. Plasmas 16, 102309 (2009); doi:10.1063/1.3250987

Published 28 October 2009

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A. P. Misra,1 N. K. Ghosh,1 and P. K. Shukla2
1Department of Mathematics, Siksha Bhavana, Visva-Bharati University, Santiniketan 731 235, India
2Institut für Theoretische Physik IV, Fakultät für Physik und Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany
The one-dimensional oblique propagation of large amplitude magnetohydrodynamic (MHD) waves in a high-beta quantum Hall-MHD plasma is studied with electron spin-1/2 effects. The plasma beta becomes high by the condition for the nonrelativistic fluid model to be valid and the condition for the collective effects to be important in quantum plasmas. Such a high-beta value is a prerequisite for large perturbations of the perpendicular magnetic field comparable with the longitudinal magnetic field. It is shown that the nonlinear evolution of such waves is described by a derivative nonlinear Schrödinger (DNLS) equation. It is found that the DNLS equation does not depend on the higher order quantum coupling associated with the Bohm potential, rather the pressure such as spin force plays the crucial role. Such an evolution equation is shown to admit spin-modified localized envelope solitons whose width L is reduced by epsilon2/v<sub>B</sub><sup>2</sup> and the amplitude increases with increasing epsilon2/v<sub>B</sub><sup>2</sup> values, where epsilon is the temperature normalized Zeeman energy and v<sub>B</sub><sup>2</sup> is the electron thermal energy normalized by the Alfvén wave energy. Moreover, the MHD waves are found to be modulationally unstable for a wave number exceeding its critical value, which typically depends on epsilon2/v<sub>B</sub><sup>2</sup>. The growth rate of the modulational instability is also investigated. Furthermore, the effect of dissipation due to plasma resistivity is shown to exhibit envelope shocklike structures instead of envelope solitons. The present nonlinear excitations can account for large scale structures in dense astrophysical plasma environments. ©2009 American Institute of Physics
History: Received 24 August 2009; accepted 29 September 2009; published 28 October 2009
Permalink: http://link.aip.org/link/?PHPAEN/16/102309/1
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KEYWORDS and PACS

Keywords
PACS
  • 52.35.Bj
    Plasma magnetohydrodynamic waves
  • 52.30.Cv
    Plasma magnetohydrodynamics
  • 52.35.Sb
    Plasma solitons; BGK modes
  • 52.35.Py
    Plasma macroinstabilities (hydromagnetic)
  • 52.25.Fi
    Plasma transport properties
  • YEAR: 2009

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PUBLICATION DATA

ISSN:
1070-664X (print)   1089-7674 (online)
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