Theoretical models for MHD turbulence in the solar wind.

Details Theoretical models for MHD turbulence in the solar wind. Theoretical models for MHD turbulence in the solar wind.

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997ncimc..20..859v&link_type=abstract

Nuovo Cimento C, Vol. 20C, N. 6, p. 859 - 869

Physics

Space Physics

Magnetohydrodynamics: Solar Wind, Magnetohydrodynamics: Plasma

Scientific paper

In situ measurements of velocity, magnetic field, density and temperature fluctuations performed in the solar wind have greatly improved our knowledge of MHD turbulence not only from the point of view of space physics but also from the more general point of view of plasma physics. Many fundamental processes in plasma physics, which were largely unknown or not understood before observations in the solar wind, have been explained, by building analytical models or performing numerical simulations. The authors discuss analytical theories and numerical simulations and outline the limits implicit in any analysis which considers the low-frequency solar-wind fluctuations as a superposition of linear modes. The characterization of low-frequency fluctuations during Alfvénic periods, which results from the models discussed, is finally presented.

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