Acceleration of the Solar Wind: a Review of Kinetic Collisionless (Exospheric) Models

Details Acceleration of the Solar Wind: a Review of Kinetic Collisionless (Exospheric) Models Acceleration of the Solar Wind: a Review of Kinetic Collisionless (Exospheric) Models

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh22b..03z&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH22B-03

Physics

2169 Solar Wind Sources, 7509 Corona

Scientific paper

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.

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