HR: 09:10h
AN: SH21B-05 INVITED    [Abstracts]
TI: The Acceleration of the Fast Solar Wind by Reconnections Between Open Magnetic Flux and Coronal Loops
AU: * Fisk, L A
EM: lafisk@umich.edu
AF: University of Michigan, 2455 Hayward St., Ann Arbor, MI 48109, United States
AB: It is possible to develop models for the acceleration of the solar wind in which the mass flux of the solar wind is determined by the release of material during the reconnection between open magnetic flux and coronal loops, and the energy source is the subsequent relaxation to equilibrium of open flux displaced by the reconnection process. Such models, if correct and verified by observations, may provide the basis for predictive models of the solar wind, since the governing parameters that determine the final speed of the solar wind are in principle observable on the solar surface, e.g., the rate of reconnection between open field lines and coronal loops as revealed by coronal jets and X-ray bright points. This theory for the acceleration of the solar wind will be reviewed along with the role of reconnection within the theory; the parameters that need to be observed to test the theory will be discussed.
DE: 2164 Solar wind plasma
DE: 2169 Solar wind sources
DE: 7509 Corona
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting