A model for the fibril structure of normal-polarity solar prominences

C. D.C. Steele; E. R. Priest

doi:10.1007/BF00146314

A model for the fibril structure of normal-polarity solar prominences

C. D.C. Steele^*, E. R. Priest

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

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.

Original language	English
Pages (from-to)	289-306
Number of pages	18
Journal	Solar Physics
Volume	140
Issue number	2
DOIs	https://doi.org/10.1007/BF00146314
Publication status	Published - Aug 1992

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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.",

author = "Steele, {C. D.C.} and Priest, {E. R.}",

year = "1992",

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AB - 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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A model for the fibril structure of normal-polarity solar prominences

Abstract

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