HR: 0830h
AN: SH21B-0159    [PDF]
TI: Radial Evolution of the Non-thermal Character of Electron Distribution Functions in the Solar Wind
AU: * Maksimovic, M
EM: milan.maksimovic@obspm.fr
AF: LESIA & CNRS, Observatoire de Paris, Pl. Jules Janssen, Meudon, 92195 France
AU: Zouganelis, I
EM: Ioannis.Zouganelis@obspm.fr
AF: LESIA & CNRS, Observatoire de Paris, Pl. Jules Janssen, Meudon, 92195 France
AU: Chaufray, J
EM: chaufrj3@cti.ecp.fr
AF: LESIA & CNRS, Observatoire de Paris, Pl. Jules Janssen, Meudon, 92195 France
AU: Issautier, K
EM: Karine.Issautier@obspm.fr
AF: LESIA & CNRS, Observatoire de Paris, Pl. Jules Janssen, Meudon, 92195 France
AU: Scime, E
EM: escime@wvu.edu
AF: Department of Physics, West Virginia University, Hodges Hall Box 6315, Morgantown, WV 26506 United States
AU: Littleton, J
EM: John.littleton@mail.wvu.edu
AF: Department of Physics, West Virginia University, Hodges Hall Box 6315, Morgantown, WV 26506 United States
AU: Salem, C S
EM: salem@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California Berkeley, 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Marsch, E
EM: marsch@linmpi.mpg.de
AF: Space Science and Engineering Division Southwest Research Institute, P.O. Drawer 28510, San Antonio, TX 78228-0510 United States
AU: Elliott, H
EM: helliott@swri.edu
AF: Max-Planck-Institut fur Aeronomie, Max-Planck-Strasse 2, Katlenburg-Lindau, 37191 Germany
AU: McComas, D J
EM: DMcComas@swri.edu
AF: Max-Planck-Institut fur Aeronomie, Max-Planck-Strasse 2, Katlenburg-Lindau, 37191 Germany
AU: Lin, R P
EM: boblin@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California Berkeley, 7 Gauss Way, Berkeley, CA 94720-7450 United States
AB: 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.
DE: 2164 Solar wind plasma
DE: 2169 Sources of the solar wind
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting