The latitudinal structure of solar wind streams from radio scintillation observations

Details The latitudinal structure of solar wind streams from radio scintillation observations The latitudinal structure of solar wind streams from radio scintillation observations

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979stin...8024242a&link_type=abstract

The latitudinal structure of solar wind streams from radio scintillation observations AFGL

Computer Science

Scintillation Counters, Solar Wind, Solar Wind Velocity, Solar Corona, Solar Magnetic Field, Sunspot Cycle, Velocity Measurement

Scientific paper

A comparison of spacecraft and IPS(Interplanetary Scintillations) measurements of the solar wind velocity for 1973-75 are presented, when the large scale velocity structure was very stable. From this comparison we infer a prototype distribution across a high speed stream for the electron density fluctuations, delta ne, in the spatial frequency range 1/10,000 - 1/100/km. The 'microturbulence' is more closely related to the velocity structure in a stream than to the bulk density; enhancements in delta ne occur wherever high speed wind overtakes low speed wind. The distribution of delta ne is closely matched by the distribution of magnetic field fluctuations approx. 1/1,000,000 km.

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