Evidence for slow mode MHD turbulence in the solar wind - Post-slow shock observations at 0.31 AU

Details Evidence for slow mode MHD turbulence in the solar wind - Post-slow shock observations at 0.31 AU Evidence for slow mode MHD turbulence in the solar wind - Post-slow shock observations at 0.31 AU

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jgr....9213653r&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 92, Dec. 1, 1987, p. 13653-13657.

Physics

5

Landau Factor, Magnetohydrodynamic Turbulence, Shock Waves, Solar Magnetic Field, Solar Wind, Frequency Ranges, Low Frequencies, Spectrum Analysis

Scientific paper

Power and coherence spectral analysis of the Helios high time resolution solar wind plasma and magnetic field observations were used to provide direct observational evidence for slow-mode MHD turbulence in the solar wind in the frequency range below about 0.005 Hz. In addition, direct observational proof is provided of the resuts of the Hada and Kennel (1985) theoretical analysis concerning nonlinear evolution of slow waves in the solar wind. It is also shown that the MHD turbulence upstream is predominantly Alfvenic and is propagating away from the sun. Thus, a first example is presented of an interplanetary slow shock where the turbulence upstream and downstream appear to be completely different in nature.

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