Radial Evolution of the Electron Distribution Functions of the Fast Solar Wind Combining Measurements From the HELIOS, WIND and ULYSSES Spacecraft

Details Radial Evolution of the Electron Distribution Functions of the Fast Solar Wind Combining Measurements From the HELIOS, WIND and ULYSSES Spacecraft Radial Evolution of the Electron Distribution Functions of the Fast Solar Wind Combining Measurements From the HELIOS, WIND and ULYSSES Spacecraft

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh21a..08z&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH21A-08

Other

2114 Energetic Particles, Heliospheric (7514), 2169 Sources Of The Solar Wind, 7509 Corona, 7513 Coronal Mass Ejections, 7514 Energetic Particles (2114)

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. Various processes like scattering of strahl electrons by shocks, corotating interaction regions or other wave/particle interactions have been invoked. We look for possible observational constraints on these processes by examining the radial evolution of the different 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.

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