Abstract
A normal-polarity prominence is modelled as a series of cool fibrils set in the hotter corona. Equations of magnetostatic equilibrium are solved and each fibril corresponds to a dip in the mgnetic field. The ratio of fibril width to interfibril spacing is dependent on the prominence-coronal temperature ratio and the ratio of plasma to magnetic pressure. The prominence mass is found to depend on the square of the magnetic field strength. When variations along the prominence are allowed in addition to those across the prominence, an apparently random pattern of fibrils results.
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Steele, C.D.C., Priest, E.R. A model for the fibril structure of normal-polarity solar prominences. Sol Phys 140, 289–306 (1992). https://doi.org/10.1007/BF00146314
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DOI: https://doi.org/10.1007/BF00146314