Computer Science – Numerical Analysis
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...420l..41a&link_type=abstract
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 420, no. 1, p. L41-L44
Computer Science
Numerical Analysis
113
Magnetic Field Configurations, Photosphere, Polarity, Shear, Solar Corona, Solar Magnetic Field, Solar Prominences, Stellar Models, Computerized Simulation, Magnetohydrodynamics, Numerical Analysis
Scientific paper
A model is presented which accounts for the formation of coronal magnetic field lines with the appropriate 'dipped' structure to support prominences. The critical ingredients of the model are that the prominence magnetic field is a truly three-dimensional structure with significant variation along the prominence length, and the magnetic field is strongly sheared near the photospheric neutral line. Numerical calculations are presented which demonstrate that these two features lead to dip formation. In addition our model is able to account for the long-puzzling observation of inverse polarity in quiescent prominences.
Antiochos Spiro K.
Dahlburg Russell B.
Klimchuk James A.
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