Abstract Our understanding of the solar wind is based upon Parker's description of a thermally driven subsonic - supersonic outflow from a fully ionized electron-proton corona. The basic physical processes of thermally driven solar wind models are discussed. We also study the effect of alpha particles in the corona on the solar wind proton flux, and further discuss the acceleration of the solar wind by Alfvén waves.
Solar wind models
Advances in Space Research ; 11 , 1 ; 197-211
1991-01-01
15 pages
Article (Journal)
Electronic Resource
English
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