Alfven waves in the solar corona and solar wind

Details Alfven waves in the solar corona and solar wind Alfven waves in the solar corona and solar wind

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994adspr..14..123v&link_type=abstract

Advances in Space Research, vol. 14, no. 4, p. (4)123-(4)133

Computer Science

2

Magnetohydrodynamic Turbulence, Magnetohydrodynamic Waves, Plasma Heating, Solar Corona, Solar Wind, Solar Wind Velocity, Solar Atmosphere, Solar Corpuscular Radiation, Velocity Measurement, Wave Propagation

Scientific paper

In situ solar wind measurements of magnetohydrodynamic (MHD) turbulence first showed, 20 years ago, that Alfven 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.

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