Physics – Plasma Physics
Scientific paper
Aug 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987esasp.275...11l&link_type=abstract
In ESA, Proceedings of the 21st ESLAB Symposium on Small Scale Plasma Processes in the Solar Chromosphere/Corona, Interplanetary
Physics
Plasma Physics
2
Magnetohydrodynamic Waves, Plasma Physics, Solar Corona, Solar Wind, Astronomical Models, Energy Budgets, Particle Acceleration, Plasma-Electromagnetic Interaction, Soho Mission
Scientific paper
Parker's thermally driven solar wind model is reviewed. The model can describe the quiet solar wind quite well, but energy must be added to the flow to drive high speed streams. It is argued that the Solar and Heliospheric Observatory (SOHO) should be used to study possible acceleration mechanisms of the solar wind, in particular acceleration by magnetohydrodynamic (MHD) waves. In the inner corona a nonnegligible wave energy flow introduces a substantial nonthermal broadening of lines from heavy ions. Simultaneous observations of line widths and of the corona density profile in the source region of the solar wind, as well as the flow emanating from that region, should lead to a better understanding of the energy balance in the solar wind.
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