Alfven waves in the solar corona and solar wind
Abstract
In 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.
- Publication:
-
Advances in Space Research
- Pub Date:
- April 1994
- DOI:
- 10.1016/0273-1177(94)90171-6
- Bibcode:
- 1994AdSpR..14d.123V
- Keywords:
-
- Magnetohydrodynamic Turbulence;
- Magnetohydrodynamic Waves;
- Plasma Heating;
- Solar Corona;
- Solar Wind;
- Solar Wind Velocity;
- Solar Atmosphere;
- Solar Corpuscular Radiation;
- Velocity Measurement;
- Wave Propagation;
- Solar Physics