The rapid motion of filaments in solar active regions

Details The rapid motion of filaments in solar active regions The rapid motion of filaments in solar active regions

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64..825m&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, July-Aug. 1987, p. 825-834. In Russian.

Astronomy and Astrophysics

Astronomy

5

Equations Of Motion, Solar Activity, Solar Prominences, Potential Theory, Solar Corona, Solar Magnetic Field

Scientific paper

Static magnetic field distribution above the photosphere surface is given, as a rule, by the solution of the potential theory problem called Neuman problem. The results are applied to the filament "activating" phenomenon of November 2, 1980. It is shown that filament motion can be described by the drift, and that there exists correspondence between the observed distribution of the flare brightness and the isolines of the Pointing vector z-component.

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