Other
Scientific paper
Nov 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...233.1005p&link_type=abstract
Astrophysical Journal, Part 1, vol. 233, no. 3, Nov. 1, 1979, p. 1005-1015.
Other
4
Magnetic Flux, Magnetohydrodynamic Stability, Solar Activity, Sunspots, Fluid Boundaries, Heat Transfer Coefficients, Reflectance, Solar Flux, Surface Waves, Turbulence Effects
Scientific paper
The dynamical properties of convective overstability in a vertical magnetic field with a downdraft are considered. A variety of effects is illustrated. The overstability produces Alfven waves propagating both upward or downward along the magnetic field. The favored direction of emission may be upward or downward depending upon the magnitude of the heat transport coefficient. The largest asymmetry is produced by a difference in reflectivity between the upper and lower boundaries. It is shown that a very modest reflection coefficient of the upper boundary, with no reflection at the lower boundary, causes most of the waves to be emitted downward, and vice versa. Applying these results to the flux tubes extending up through the convective zone of the Sun, it follows that those flux tubes are dynamically active beneath the surface, as suggested earlier by ourselves and others, but there is no reason to expect any significant wave flux to appear in the field above the surface. The waves propagate downward into the Sun and are presumably dispersed there by the nonlinear interaction with the turbulent convection, etc.
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