Small scale MHD wave processes in the solar atmosphere and solar wind

Details Small scale MHD wave processes in the solar atmosphere and solar wind Small scale MHD wave processes in the solar atmosphere and solar wind

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987esasp.275..161h&link_type=abstract

In ESA, Proceedings of the 21st ESLAB Symposium on Small Scale Plasma Processes in the Solar Chromosphere/Corona, Interplanetary

Physics

10

Magnetohydrodynamic Waves, Plasma Waves, Solar Atmosphere, Solar Wind, Cyclotron Resonance, Eddy Viscosity, Plasma Turbulence, Plasma-Particle Interactions, Solar Corona, Spicules

Scientific paper

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.

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