Radial evolution of solar wind thermal electron distributions due to expansion and collisions

Details Radial evolution of solar wind thermal electron distributions due to expansion and collisions Radial evolution of solar wind thermal electron distributions due to expansion and collisions

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....95.4217p&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 95, April 1, 1990, p. 4217-4228. Research sponsored by DOE.

Other

37

Electron Distribution, Electron Scattering, Hot Electrons, Satellite Observation, Solar Wind, Interplanetary Magnetic Fields, Particle Collisions, Solar Electrons

Scientific paper

ISEE 3 electron observations near 1 AU show that the solar wind thermal electron temperature anisotropy, T(parallel)/T(perpendicular), is typically 1.0 to 1.5, with densest distributions most nearly isotropic, but is sometimes much higher when density is low. For a small observational subset characterized by high density and low bulk speed, T(perpendicular) can exceed T(parallel). Based on these and other observations, a simple model is proposed for radial evolution of thermal electrons in a structureless solar wind under the influence of Coulomb collisions and geometric expansion in a spiral interplanetary magnetic field. The model, which satisfactorily explains the 1 AU observations, shows that the evolution of electron temperature and T(parallel)/T(perpendicular) is controlled by plasma density, flow speed, and initial temperature, with density the most important factor. The model makes predictions for radial distances other than 1 AU and for high solar latitudes.

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