The understanding of the solar wind is based upon Parker's (1958) 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. Also studied are the effect of alpha particles in the corona on the solar wind proton flux. The acceleration of the solar wind by Alfven waves is discussed.
Solar wind models
Advances in Space Research ; 11 , 1 19
1991-01-01
Miscellaneous
No indication
English
Elsevier | 1991
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