Physics
Scientific paper
Nov 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.348..201a&link_type=abstract
In ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition p 201-2
Physics
1
Mathematical Models, Solar Corona, Solar Magnetic Field, Solar Physics, Solar Prominences, Stellar Models, Astronomical Models, Chromosphere, Star Formation, Stellar Structure, Sun
Scientific paper
The outstanding questions on the formation of quiescent prominences are discussed. One key issue is identified to be the formation of dips in coronal magnetic field lines. A model is presented which can account for such dipped field lines. 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 has strong shear concentrated at the photospheric neutral line. Simulations which demonstrate that these two features lead to dip formation and that the geometry of the dips are such that inverse polarity prominences can be explained are presented. Another key issue is identified to be the formation of prominence condensations on dipped field lines. It is argued that a spatially varying coronal heating rate which is maximum near the chromosphere explain these condensations.
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