Physics
Scientific paper
Dec 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....9520673m&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 95, Dec. 1, 1990, p. 20673-20683.
Physics
283
Magnetohydrodynamic Turbulence, Magnetohydrodynamic Waves, Solar Wind, Two Dimensional Flow, Solar Cosmic Rays, Turbulence Models, Wave Interaction, Wentzel-Kramer-Brillouin Method
Scientific paper
Assuming that the slab and isotropic models of solar wind turbulence need modification (largely due to the observed anisotropy of the interplanetary fluctuations and the results of laboratory plasma experiments), this paper proposes a model of the solar wind. The solar wind is seen as a fluid which contains both classical transverse Alfvenic fluctuations and a population of quasi-transverse fluctuations. In quasi-two-dimensional turbulence, the pitch angle scattering by resonant wave-particle interactions is suppressed, and the direction of minimum variance of interplanetary fluctuations is parallel to the mean magnetic field. The assumed incompressibility is consistent with the fact that the density fluctuations are small and anticorrelated, and that the total pressure at small scales is nearly constant.
Goldstein Melvyn L.
Matthaeus William H.
Roberts Daniel A.
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