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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.


We conjecture a relationship between this phenomenon and the observed spatiotemporal intermittancy of the oscillations. By contrast, in regions where the field is close to vertical, the waves continue to propagate upward, channeled along the field lines but otherwise largely unaffected by the field.

Dr Bertil F Dorch
Syddansk Universitet

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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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