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Paper: The Internal Structures and Dynamics of Solar Quiescent Prominences
Volume: 346, Large-scale Structures and their Role in Solar Activity
Page: 211
Authors: Petrie, G.; Low, B.
Abstract: We present generalized Kippenhahn-Schlüter (KS) equilibrium solutions of the magnetohydrodynamic (MHD) equations, constructed of arrays of laminated isothermal (KS) prominence sheets whose temperatures, sag angles and dip positions may vary arbitrarily from sheet to sheet. This great versatility allows us to model the filamentary structure of prominences and illustrate why their observed dimensions differ from their characteristic hydrostatic scale lengths. We also apply these equilibria to investigate the role of internal prominence motions in solar magnetism. The solar corona is continually being injected with magnetic flux from the solar interior, flux that cannot be annihilated in bulk by the electrically highly conducting corona. Ascending small-scale structures as well as large-scale eruptions of prominences may both serve to carry excess magnetic flux out of the corona. This process is investigated with an interest in the dissipation of tangential discontinuities forming spontaneously in the supporting magnetic field of a prominence. The net effect of the magnetic reconnection is a downflow of mass accompanied by an upward transport of magnetic flux. This effect may play an important, direct and indirect, role in ejecting magnetic flux from the corona into interplanetary space. Thin counter-streaming layers of prominence plasma predicted by this work have already been observed.
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