Enhanced emission of Alfven waves from sunspots during proton flares

Details Enhanced emission of Alfven waves from sunspots during proton flares Enhanced emission of Alfven waves from sunspots during proton flares

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981soph...70..381m&link_type=abstract

Solar Physics, vol. 70, Apr. 1981, p. 381-393.

Physics

2

Chromosphere, Magnetohydrodynamic Waves, Solar Corona, Solar Flares, Solar Protons, Sunspots, Solar Flux, Solar Granulation, Solar Magnetic Field, Umbras

Scientific paper

It is known that in many proton flares, chromospheric emission overlies the umbra of a sunspot, which indicates that the transition region (TR) between chromosphere and corona in the umbral flux tube has moved down to lower altitudes. Because of this lowering, umbral Alfven waves have readier access to the corona; this coronal leakage depends exponentially on the altitude of the TR. It is found that the Alfven wave flux that leaks out of the umbra into the corona can exceed 10-million ergs/sq cm-s. A flux of this magnitude is expected to dissipate rapidly in the corona, thus contributing to a positive feedback loop which ensures prolonged (about 1-hr) leakage of the umbral Alfven waves into the corona. It is suggested that these Alfven waves may contribute significantly to prolonged energization of proton flares in which umbral coverage occurs.

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