Magneto-atmospheric waves

Details Magneto-atmospheric waves Magneto-atmospheric waves

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..129..201a&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 129, Oct. 1990, p. 201-219.

Physics

10

Magnetohydrodynamic Waves, Solar Atmosphere, Solar Oscillations, Atmospheric Models, Gravity Waves, Magnetic Field Configurations, Magnetoacoustic Waves, Solar Interior, Solar Magnetic Field

Scientific paper

The nature and properties of magneto-atmospheric (MA) waves are discussed. A simple model atmosphere, isothermal and permeated by a uniform vertical magnetic field, was used to find that there are two types of modes with avoided crossing of the eigencurves in a K-Omega diagram. The properties of these waves are found to be identical to the uncoupled fast and slow MA waves away from the crossings (specially for small horizontal wavenumber, K much less than 1). The energy density for the fast modes is found to vanish with height and is responsible for the 3-min umbral oscillations, while the slow mode energy density is harmonic.

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