Physics
Scientific paper
Dec 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980soph...68..279n&link_type=abstract
Solar Physics, vol. 68, Dec. 1980, p. 279-295. Research supported by the National Center for Atmospheric Research.
Physics
13
Magnetohydrodynamic Waves, Solar Magnetic Field, Sunspots, Wave Propagation, Lines Of Force, Solar Atmosphere, Stellar Models, Temperature Effects, Wave Equations
Scientific paper
The propagation of Alfven waves in a simple model of a sunspot is considered. The vertical structure near the center of the umbra is modeled realistically, but the horizontal structure is not considered. The full wave equation is solved, without recourse to the WKB approximation. Only wave propagation in the vicinity of the central field line in an axisymmetric spot is examined, and it is assumed that this field line is open. By taking wave reflections into account, the observations of nonthermal motions near the temperature minimum (Beckers, 1976) and in the corona (Beckers and Schneeberger, 1977) are found to be consistent with an upward-propagating Alfvenic energy flux density of a few times 10 to the 7th erg/sq cm/sec. This flux density is too small to cool the sunspot, but large enough to supply the energy requirements of the transition region and corona above a sunspot. This conclusion depends on the assumptions that the observed motions are indeed Alfvenic with periods near 180 sec.
Hollweg Joseph V.
Nye Alan H.
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