HR: 16:05h
AN: SH24A-03    [Abstracts]
TI: Predicting the Solar Wind
AU: * Fisk, L A
EM: lafisk@umich.edu
AF: Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109
AU: Gloeckler, G
EM: gg10@umail.umd.edu
AF: Institute of Physical Science and Technology, Department of Physics, University of Maryland, College Park, MD 20742
AU: Zurbuchen, T H
EM: thomasz@engin.umich.edu
AF: Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109
AB: A theory has been developed for the acceleration of the solar wind, which couples the acceleration to the behavior of the open magnetic flux of the Sun. The open flux is transported in the corona by various diffusive processes, which in turn can impart energy into and accelerate the solar wind. The theory thus provides an opportunity to relate the final speed of the solar wind to the processes governing the behavior of the open flux, or equivalently, it provides the basis for predicting the solar wind flow from observed solar parameters. Comparison of the results of this approach with observations, and the relationship of this theory with other methods to predict the solar wind will be considered.
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly