Physics
Scientific paper
May 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...85...97c&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 85, May 1983, p. 97-111. Research supported by the Science and Engineering Research Council
Physics
6
Chromosphere, Magnetohydrodynamic Waves, Penumbras, Photosphere, Wave Propagation, Astronomical Models, Shear Flow, Solar Corona, Solar Magnetic Field, Wave Equations
Scientific paper
The full magnetoatmospheric wave equation is numerically solved for the particular penumbral model of Nye and Thomas (1974). For chromospheric running penumbral waves it is found that the maximum vertical velocity occurs at the base of the H-alpha region, much lower than previous WKB estimates have suggested. The maximum 'vertical' kinetic energy occurs at about -130 km along the z direction. An attempt is made to interpret photospheric events in the context of a simplified linear theory; a high vertical velocity maximum is found in the corona, and the modes appear highly dispersive for periods of 220 s or greater. Finally a preliminary attempt is made to model some aspects of the Evershed flow in sunspot penumbrae, in particular to find what effect such vertically sheared motions have on the discussed eigenvalues and eigenfunctions. The former are found to change little, while the latter are significantly distorted.
Adam John A.
Cally Paul S.
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