The radial evolution of the solar wind, 1-10 AU

Details The radial evolution of the solar wind, 1-10 AU The radial evolution of the solar wind, 1-10 AU

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280.509g&link_type=abstract

In JPL Solar Wind Five p 509-519 (SEE N84-13067 03-92)

Computer Science

2

Interplanetary Magnetic Fields, Solar Wind, Solar Wind Velocity, Comparison, Helios Project, Interstellar Matter, Pioneer Space Probes, Protons, Shock Waves, Variations, Voyager Project

Scientific paper

The interplanetary plasma and magnetic field observations from 1 to 10 AU are reviewed. Over this distance no clear reduction in average speed is seen. The range of wind speeds becomes smaller though high speed streams are still observed. The density, temperature and magnetic field profiles become dominated by the large values seen in the co-rotating interaction regions. The temperature falls more slowly than would be expected from a simple, adiabatic model. Co-rotating shocks appear beyond approximately 3 AU in Voyager data as opposed to beyond approximately 1.5 AU in the Pioneer data. Reverse shocks appear later than forward shocks; reverse shocks do not begin to appear until approximately 4 AU; reverse shocks appear to decay more rapidly than forward shocks. No clear effect due to interaction with the interstellar medium was seen in this radial range.

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