Working Group 1 Report: Solar Wind Models from the Sun to 1 AU: Constraints by "in situ" and Remote Sensing Measurements |
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Authors: | E Leer E Marsch |
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Institution: | (1) Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029, N-0316 Oslo, Norway;(2) Max Planck Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany |
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Abstract: | The goal of Working Group 1 was to discuss constraints on solar wind models. The topics for discussion, outlined by Eckart
Marsch in his introduction, were: (1) what heats the corona, (2) what is the role of waves, (3) what determines the solar
wind mass flux, (4) can stationary, multi-fluid models describe the fast and slow solar wind, or (5) do we need time dependent
fluid models, kinetic models, and/or MHD models to describe solar wind acceleration.
The discussion in the working group focused on observations of "temperatures" in the corona, mainly in coronal holes, and
whether the observations of line broadening should be interpreted as thermal broadening or wave broadening. Observations of
the coronal electron density and the flow speed in coronal holes were also discussed. There was only one contribution on observations
of the distant solar wind, but we can place firm constraints on the solar wind particle fluxes and asymptotic flow speeds
from observations with Ulysses and other spacecraft. Theoretical work on multi-fluid models, higher-order moment fluid models,
and MHD models of the solar wind were also presented.
This revised version was published online in June 2006 with corrections to the Cover Date. |
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