Physics
Scientific paper
Dec 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286..295c&link_type=abstract
In ESA, Seismology of the Sun and Sun-Like Stars p 295-300 (SEE N89-25819 19-92)
Physics
Frequency Measurement, Magnetohydrodynamic Waves, Solar Atmosphere, Wave Propagation, Data Acquisition, Magnetohydrostatics, Shock Waves, Solar Magnetic Field, Solar Physics
Scientific paper
The propagation of Alfven waves in a viscous and resistive atmospheric layer, in isothermal magnetohydrostatic equilibrium, with constant rate of ionization, under a horizontal magnetic field, either uniform or decaying with altitude is considered. The wave equation relevant to these two cases is derived, and its solution in terms of hypergeometric functions is used to plot wave amplitude and phase versus altitude for several values of wave frequency, horizontal wavenumber, and viscous and resistive damping. It is shown that: (1) the amplitudes initially grow due to reducing mass density and the decay due to dissipation, i.e., go through a maximum; (2) the phases also go through a maximum, i.e., upward propagating waves are reflected downward; (3) amplitude and phase changes are smaller in a flux tube than in a uniform magnetic field, because in the former case the magnetic field decays, as the flux tube fans out with height.
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