Spectral and spatial evolution of compressible turbulence in the inner solar wind

Details Spectral and spatial evolution of compressible turbulence in the inner solar wind Spectral and spatial evolution of compressible turbulence in the inner solar wind

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....9511945m&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 95, Aug. 1, 1990, p. 11945-11956.

Physics

95

Current Sheets, Magnetohydrodynamic Flow, Plasma Compression, Plasma Turbulence, Solar Wind, Helios Satellites, Plasma Currents, Spatial Distribution, Spectral Energy Distribution

Scientific paper

Magnetic field and plasma data collected by the Helios spacecraft between 0.3 and 1 AU near the activity minimum of solar cycle 21 have been analyzed to establish spectral characteristics of compressive fluctuations in the inner solar wind and their relation to the morphology of the plasma flow and magnetic field. The compressive turbulence level is found to be closely related to the stream structure or latitudinal location with respect to the heliospheric current sheet. Compressive turbulence in low-speed flows is more fully developed and intense. The spectra are radially invariant and come close to a -5/3 spectral law. In constrast, fast stream turbulence becomes increasingly compressive with increasing heliocentric distance. The spectra reveal a flatter high-frequency part, which gradually seems to get straightened out at large solar distances. Single case studies, as well as averaged spectra and their spectral features, are presented and discused in the theoretical turbulence literature.

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