Why is it important?
We find that in regions where the field is significantly inclined to the vertical, refraction by the rapidly increasing phase speed of the fast modes results in total internal reflection of the waves at a surface whose altitude is highly variable.
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This page is a summary of: Waves in the Magnetized Solar Atmosphere. I. Basic Processes and Internetwork Oscillations, The Astrophysical Journal, January 2002, American Astronomical Society, DOI: 10.1086/324214.
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Waves in the Magnetized Solar Atmosphere. II. Waves from Localized Sources in Magnetic Flux Concentrations
Numerical simulations of wave propagation in a two-dimensional stratified magneto-atmosphere are presented for conditions that are representative of the solar photosphere and chromosphere. Both the emergent magnetic flux and the extent of the wave source are spatially localized at the lower photospheric boundary of the simulation.
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