Microturbulence in solar wind streams

Details Microturbulence in solar wind streams Microturbulence in solar wind streams

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980jgr....85.6025a&link_type=abstract

Journal of Geophysical Research, vol. 85, Nov. 1, 1980, p. 6025-6030.

Computer Science

Sound

29

Electron Density (Concentration), Plasma Turbulence, Satellite Sounding, Scintillation, Solar Wind Velocity, Magnetohydrodynamic Waves, Proton Energy

Scientific paper

A comparison of spacecraft and IPS measurements of the solar wind velocity for 1973-75, when the large scale velocity structure was very stable is presented. A prototype distribution across a high-speed stream for the electron density fluctuations in the spatial frequency range 0.0001 to 0.01/km is inferred. Enhancements of the electron density fluctuations occur in the stream interaction region, but they are not as large as those of np and they peak 12 hours after the np peak. The distribution of the electron density fluctuations is similar to that of the large scale magnetic field fluctuations, but the electron density fluctuations also show a broad variation. Overall, the electron density fluctuations are most closely matched to the positive velocity gradient at the leading edge of a stream.

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