Other
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh21b0159m&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #SH21B-0159
Other
2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind
Scientific paper
Observed electron distribution functions of the solar wind permanently exhibit three different components : a thermal core and a supra-thermal halo, which are always present at all pitch angles, and a sharply magnetic field aligned "strahl" which is usually antisunward-moving. If the Coulomb collisions could explain the relative isotropy of the core population, the origin of the halo population and more specifically the origin of its sunward-directed part remains unknown. Processes invoking scattering of strahl electrons by shocks, corotating interaction regions or other wave/particle interactions have been invoked. We look for possible observationnal constraints on these processes by examining the radial evolution of the various populations of the electron distribution functions in the solar wind. For this purpose we combine HELIOS (0.3 to 0.7 AU), WIND (1 AU) and ULYSSES (1.3 to 3 AU) observations performed during fast solar wind periods at minimum of activity.
Chaufray J.
Elliott Heather
Issautier Karine
Lin Robert P.
Littleton J.
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