On the radial evolution of MHD turbulence in the inner heliosphere

Details On the radial evolution of MHD turbulence in the inner heliosphere On the radial evolution of MHD turbulence in the inner heliosphere

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....95.8211m&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 95, June 1, 1990, p. 8211-8229.

Physics

139

Cross Correlation, Heliosphere, Magnetohydrodynamic Turbulence, Solar Wind, Autocorrelation, Magnetohydrodynamic Waves, Power Spectra, Spectroheliographs, Wentzel-Kramer-Brillouin Method

Scientific paper

MHD fluctuations in the solar wind are reanalyzed here using Elsanic domain are more transverse in the perihelion, they radially evolve toward an equipartition of the energy in the three spatial dimensions at larger heliocentric distances. The e- spectrum does not change a lot at low frequencies but strongly steepens beyond about 0.0002 Hz. The spectra results on e- suggest that isotropic turbulence with an index of -5/3 is probably the ultimate state toward which solar wind MHD fluctuations evolve.

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