HR: 11:00h
AN: SH22B-03    [Abstracts]
TI: Acceleration of the Solar Wind: a Review of Kinetic Collisionless (Exospheric) Models
AU: * Zouganelis, I
EM: ioannis.zouganelis@obspm.fr
AF: LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 place Jules Janssen, Meudon, 92190, France
AU: Maksimovic, M
EM: milan.maksimovic@obspm.fr
AF: LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 place Jules Janssen, Meudon, 92190, France
AU: Meyer-Vernet, N
EM: nicole.meyer@obspm.fr
AF: LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 place Jules Janssen, Meudon, 92190, France
AU: Issautier, K
EM: karine.issautier@obspm.fr
AF: LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 place Jules Janssen, Meudon, 92190, France
AU: Landi, S
EM: slandi@arcetri.astro.it
AF: Dipartimento di Astronomia e Scienza dello Spazio, University of Florence, Largo Enrico Fermi 2, Firenze, 50125, Italy
AU: Pantellini, F
EM: filippo.pantellini@obspm.fr
AF: LESIA, Observatoire de Paris, CNRS, UPMC, Universite Paris Diderot, 5 place Jules Janssen, Meudon, 92190, France
AU: Lamy, H
EM: herve.lamy@oma.be
AF: Belgian Institute for Space Aeronomy, 3 Avenue Circulaire, Brussels, 1180, Belgium
AB: One of the basic properties of the solar wind, that is the high speed of the fast wind, is still not self-consistently explained. This is mainly due to the theoretical difficulty of treating weakly collisional plasmas. The fluid approach implies that the medium is collision dominated and that the particle velocity distributions are close to Maxwellians. However the electron velocity distributions observed in the solar wind depart significantly from Maxwellians, indicating the limited validity of this hypothesis. In this work, we present a review of exospheric models that assume electron velocity distributions in the corona with suprathermal tails, but make no assumption on the heat flux, which is calculated self-consistently. We show how the recent developments of these models achieve to predict the fast solar wind without assuming an unreasonably large corona temperature and without additional heating of the outer region of the corona. We finally show the limitations of the present models and outline the basic perspectives for future research.
DE: 2169 Solar wind sources
DE: 7509 Corona
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting