Model for the fibril structure of solar prominences

Details Model for the fibril structure of solar prominences Model for the fibril structure of solar prominences

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...225..213b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 225, no. 1, Nov. 1989, p. 213-221. Research supported by the Ministry of Scien

Physics

28

Fine Structure, Magnetohydrodynamics, Solar Limb, Solar Prominences, Solar Activity, Solar Magnetic Field, Solar Physics, Stellar Models

Scientific paper

Limb observations of quiescent solar prominences have revealed them to be composed of many fine structures. Also observations in H-alpha and UV lines suggest that quiescent filaments are made up of many clusters of small-scale loops at different temperatures inclined to the filament axis, with the C IV structures more extended than the H-alpha ones. In H-alpha, the dimensions of these structures are about 7000 km long and 1000 km thick, and they evolve over a typical time scale of about 8 min. The aim has been to take into account such observations and to construct a model for the fibril structure of solar prominences in terms of slender magnetic flux tubes, in which the main observed parameters of both quiescent and active-region prominences are reproduced.

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