Physics
Scientific paper
May 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985svmf.nasa...86f&link_type=abstract
In NASA. Marshall Space Flight Center Meas. of Solar Vector Magnetic Fields p 86-100 (SEE N85-29869 18-92)
Physics
Magnetic Flux, Magnetohydrodynamic Flow, Photosphere, Solar Corona, Solar Magnetic Field, Current Distribution, Current Sheets, Electric Current, Mathematical Models, Solar Physics, Sun
Scientific paper
The resistive-MHD equations are numerically solved in two-dimensions for an initial-boundary-value problem which models the emergence of magnetic flux from the photosphere into the corona. As the emergence begins a current sheet forms around the emerging region which separates the emerging region from the overlying coronal magnetic field. This current sheet is the source of the free-magnetic energy in the system, and in the limit of zero resistivity it is a simple tangential discontinuity. However, when the resistivity is finite, reconnection between the magnetic field in the emerging region and the overlying coronal magnetic field ensures, and the subsequent evolution of the enveloping current sheet becomes complex. The overall time history of the current evolution is suggestive of the expected current evolution for the pre-flare, impulsive, and main phases of flares.
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