Numerical simulation of solar coronal magnetic fields

Details Numerical simulation of solar coronal magnetic fields Numerical simulation of solar coronal magnetic fields

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nasa.rept.....d&link_type=abstract

Interim Report National Aeronautics and Space Administration. Langley Research Center, Hampton, VA.

Other

Magnetic Field Configurations, Photosphere, Solar Activity, Solar Corona, Solar Magnetic Field, Current Sheets, Magnetic Cooling, Mathematical Models, Stellar Spectra, Time Dependence

Scientific paper

Many aspects of solar activity are believed to be due to the stressing of the coronal magnetic field by footpoint motions at the photosphere. The results are presented of a fully spectral numerical simulation which is the first 3-D time dependent simulation of footpoint stressing in a geometry appropriate for the corona. An arcade is considered that is initially current-free and impose a smooth footpoint motion that produces a twist in the field of approx 2 pi. The footprints were fixed and the evolution was followed until the field relaxes to another current-free state. No evidence was seen for any instability, either ideal or resistive and no evidence for current sheet formation. The most striking feature of the evolution is that in response to photospheric motions, the field expands rapidly upward to minimize the stress. The expansion has two important effects. First, it suppresses the development of dips in the field that could support dense, cool material. For the motions assumed, the magnetic field does not develop a geometry suitable for prominence formation. Second, the expansion inhibits ideal instabilities such as kinking. The results indicate that simple stearing of a single arcade is unlikely to lead to solar activity such as flares or prominences. Effects are discussed that might possibly lead to such activity.

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