Physical nature of the low-speed solar wind

Details Physical nature of the low-speed solar wind Physical nature of the low-speed solar wind

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996recs.conf.....g&link_type=abstract

Conference Paper, Scientific Basis for Robotic Explorations Close to the Sun

Physics

7

Solar Wind, Low Speed, Solar Activity Effects, Solar Corona, Magnetic Equator, High Speed, Wind Velocity, Wind Measurement, Density Measurement, Shear Flow, Magnetic Fields, Abundance, Cosmic Plasma, Helium

Scientific paper

In situ observations indicate that the low-speed wind is highly variable. It commonly originates on open field lines that thread coronal streamers in the vicinity of the magnetic equator, but transient ejections are also a source of low-speed flows on occasion. Close to the Sun a large flow shear probably is common at the interface between low- and high-speed flows. Near solar activity minimum low-speed flows are confined to a narrow band 40-45 deg wide centered roughly on the solar equator, but near solar maximum low-speed flows may dominate at all heliographic latitudes.

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