Small-scale MHD wave processes in the solar atmosphere and solar wind.
Abstract
Solar wind observations suggesting wave-particle interactions via ion-cyclotron resonances are reviewed. The required power at high frequencies is presumably supplied via a turbulent cascade. Tu's (1987) model, which considers a turbulent cascade explicitly, is outlined. In the solar atmosphere, resonance absorption is considered. The meanings of the cusp and Alfven resonances are discussed, and it is shown how energy gets pumped into small scales. It is shown that resonance absorption can heat the corona and spicules in a manner consistent with observations, if turbulence provides an eddy viscosity.
- Publication:
-
Small Scale Plasma Processes in the Solar Chromosphere/Corona, Interplanetary Medium and Planetary Magnetospheres
- Pub Date:
- August 1987
- Bibcode:
- 1987ESASP.275..161H
- Keywords:
-
- Magnetohydrodynamic Waves;
- Plasma Waves;
- Solar Atmosphere;
- Solar Wind;
- Cyclotron Resonance;
- Eddy Viscosity;
- Plasma Turbulence;
- Plasma-Particle Interactions;
- Solar Corona;
- Spicules;
- Solar Physics;
- Magnetohydrodynamics:Solar Atmosphere;
- Magnetohydrodynamics:Solar Wind;
- Plasma Waves:Solar Atmosphere;
- Plasma Waves:Solar Wind;
- Solar Atmosphere:Magnetohydrodynamics;
- Solar Atmosphere:Plasma Waves;
- Solar Wind:Magnetohydrodynamics;
- Solar Wind:Plasma Waves