AbstractIn situ solar wind measurements of MHD turbulence first showed, 20 years ago, that Alfvén waves propagating away from the sun are a dominant component, at least in high speed streams at solar minimum, with sufficient energy to explain the heating of the distant solar wind. Here we discuss some aspects of the propagation of these waves upward from the solar coronal base, where they are presumably generated, with particular emphasis on the effects of the large scale gradients on the transmission, the development of turbulence and wave dissipation.
Alfven waves in the solar corona and solar wind
Advances in Space Research ; 14 , 4 ; 123-133
1993-01-01
11 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
Alfvén Waves in the Solar Corona and Solar Wind
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