Solar prominences and observational programs

Details Solar prominences and observational programs Solar prominences and observational programs

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987lastr.101..321m&link_type=abstract

L'Astronomie (ISSN 0004-6302), vol. 101, May 1987, p. 321-329. In French.

Astronomy and Astrophysics

Astronomy

Solar Corona, Solar Prominences, H Alpha Line, Magnetic Field Configurations, Solar Flares, Solar Limb, Solar Magnetic Field, Stellar Mass Ejection

Scientific paper

The observed characteristics of solar prominences are reviewed, and models for the formation of filaments and for the magnetic structure of protuberances are discussed. Data suggest that coronal filaments are formed either by the pumping of chromospheric matter or by condensation of the coronal plasma itself by thermal instability. The class of Kippenhahn-Schluter models involve magnetic rings which are bent under the influence of gravity, and the class of Kuperus-Raadu models place prominences above a certain neutral point. Observations of filamentary velocity fields indicate that the magnetic support of the condensation is in quasi-static evolution. Three proposed areas of study of prominences, the connections and exchanges of matter at great distances, eruptive prominences, and the sudden disappearance of prominences, are discussed.

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