Alfven waves in the solar atmosphere

Details Alfven waves in the solar atmosphere Alfven waves in the solar atmosphere

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978soph...56..305h&link_type=abstract

Solar Physics, vol. 56, Feb. 1978, p. 305-333.

Physics

68

Magnetohydrodynamic Waves, Solar Atmosphere, Solar Wind, Wave Propagation, Atmospheric Models, Propagation Modes, Solar Flux Density, Wave Equations

Scientific paper

In this examination of Alfven wave propagation in the solar atmosphere, the full wave equation is solved without recourse to the small-wavelength eikonal approximation and the background solar atmosphere is described in terms of a HSRA/VAL representation of the photosphere and chromosphere, a 200-km thick transition region, a model for the upper transition region below a coronal hole, and the Munro-Jackson (1977) model of a polar coronal hole. It is found that the wave Poynting flux exhibits a series of strong resonant peaks whose resonant frequencies are in the ratios of the zeroes of J0. The precise periods can not be predicted and are influenced by several factors, but the Poynting flux in the resonant peaks can be large enough to affect the solar wind. The interrelations of other parameters are discussed.

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