Spatial dependences in the distant solar wind: Pioneers 10 and 11

Details Spatial dependences in the distant solar wind: Pioneers 10 and 11 Spatial dependences in the distant solar wind: Pioneers 10 and 11

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280.521s&link_type=abstract

In JPL Solar Wind Five p 521-535 (SEE N84-13067 03-92)

Mathematics

2

Interplanetary Magnetic Fields, Pioneer 10 Space Probe, Pioneer 11 Space Probe, Solar Magnetic Field, Solar Wind, Comparison, Mathematical Models, Proton Density (Concentration), Solar Cycles, Solar Wind Velocity, Variations

Scientific paper

Pioneer 10, 11 observations of the solar wind and magnetic field between 1 and 20 AU are reviewed. Spatial dependences, which are emphasized, must be inferred in the presence of large temporal variations including solar cycle effects. The separation of spatial and temporal dependences is achieved principally through the use of multipoint observations including baseline measurements at 1 AU. Measurements of the solar wind parameters (radial speed, flux, proton temperature) and of the magnetic field magnitude and components are compared with two theories, the Parker theory which assumes radial, azimuthally symmetric flow and the Goldstein-Jokipii theory which includes effects associated with stream-stream interactions. The observed radial gradients in the proton density and velocity and the magnetic field are consistent with the Parker model. A qualitative dependence of field magnitude on heliomagnetic latitude, i.e., referred to the observed location of the heliospheric current sheet, was derived. The field strength was found to decrease with distance from the current sheet.

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