Physics
Scientific paper
Oct 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...88..219p&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 88, Oct. 1983, p. 219-239.
Physics
69
Lines Of Force, Magnetic Field Configurations, Solar Magnetic Field, Solar Physics, Solar Prominences, Topology, Astronomical Models, Coronal Loops, Differential Equations, Vertical Motion
Scientific paper
It is suggested that the present solar quiescent prominence model, in which the prominences are nested in a 'figure-eight' magnetic field, is the natural consequence of the distention of bipolar regions upward into the corona. If this distention is sufficiently slow for hydrostatic equilibrium to hold approximately along the field lines, the transverse gas pressure forces fall exponentially with height, while the inward Lorentz forces fall as a power law. At low coronal height, the pressure and Lorentz forces cannot balance out in those cases where the field lines remain tied to the photosphere, and an inward collapse with subsequent reconnection at the point of closest approach should then occur. Assuming that the isolated helices formed by reconnection are insulated from coronal thermal conduction and heating, the radiative cooling process and condensation is considered for the 6000-10,000 K temperature range.
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