Abstract: Stability theory has several important roles to play in describing solar prominences. Firstly, the amazing stability of the large quiescent prominences and the smaller active-region filaments must be explained and, secondly, stability theory may predict the sudden eruption of a prominence once critical conditions are reached. Thirdly, the fine structure observed in prominences may be due to localised instabilities that do not disrupt the overall magnetic field pattern. Finally, the formation and long lifetimes suggest that thermal instabilities must also be considered.
Publication Year: 1988
Publication Date: 1988-01-01
Language: en
Type: book-chapter
Indexed In: ['crossref']
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