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Eruptive solar magnetic fieldsThe quasi-steady evolution of solar magnetic fields in response to gradual photospheric changes is considered, with particular attention given to the threshold of a sudden eruption in the solar atmosphere. The formal model of an evolving, force-free field dependent on two Cartesian coordinates is extended to a field which is not force free but in static equilibrium with plasma pressure and gravity. The basic physics is illustrated through the evolution of a loop-shaped electric current sheet enclosing a potential bipolar field with footpoints rooted in the photosphere. A free-boundary problem is posed and then solved for the equilibrium configuration of the current sheet in a hydrostatically supported isothermal atmosphere. As the footpoints move apart to spread a constant photospheric magnetic flux over a larger region, the equilibria available extend the field to increasing heights.
Document ID
19820035876
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Low, B. C.
(NASA Marshall Space Flight Center Huntsville, AL, United States)
Date Acquired
August 10, 2013
Publication Date
December 1, 1981
Publication Information
Publication: Astrophysical Journal
Subject Category
Solar Physics
Accession Number
82A19411
Distribution Limits
Public
Copyright
Other

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