The latitudinal structure of solar wind from radio scintillation observations

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

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978stin...7919980k&link_type=abstract

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Physics

Radio Frequency Interference, Scintillation, Solar Corona, Solar Wind Velocity, Emission Spectra, Iron, Line Spectra

Scientific paper

The relation between the solar corona and high-speed solar wind measured from interplanetary scintillations (IPS) are investigated. Preliminary results show that regions of high coronal intensity of the 5303 A Fe XIV green line are associated with low IPS velocities, whereas regions of low intensity are associated with both low and high velocities. There is some indication at high heliographic latitudes that the IPS velocity is inversely correlated with the angular divergence of the coronal magnetic field. A new model for the turbulence profile in a solar wind stream, is presented which will be used to refine this interpretation of IPS data.

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