The evolution of coronal magnetic fields

Details The evolution of coronal magnetic fields The evolution of coronal magnetic fields

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..130..399p&link_type=abstract

(Committee of European Radio Astronomers, SNSF, URSI, et al., Workshop on Particle Beams in the Solar Atmosphere, Braunwald, Swi

Physics

14

Force-Free Magnetic Fields, Magnetic Field Configurations, Solar Corona, Solar Magnetic Field, Atmospheric Heating, Flow Velocity, Magnetic Flux, Photosphere, Solar Rotation

Scientific paper

Slow photospheric motions can produce flow speeds in the corona which are fast enough to violate quasi-static evolution. Therefore, high-speed flows observed in the corona are not necessarily due to a loss of equilibrium or stability. This paper presents an example where the flow speed increases indefinitely with height while the coronal magnetic energy increases quadratically with time.

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