Eruptive instability of cylindrical prominences

Details Eruptive instability of cylindrical prominences Eruptive instability of cylindrical prominences

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..129..295v&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 129, Oct. 1990, p. 295-312.

Physics

58

Coronal Loops, Solar Activity, Solar Prominences, Cold Plasmas, Equations Of Motion, Magnetic Field Configurations, Magnetic Field Reconnection, Magnetohydrodynamic Waves, Solar Magnetic Field

Scientific paper

The present investigation of the stability of solar prominences and the dynamics of an eruption represents the prominence as a uniformly twisted, curved magnetic tube which is anchored at both ends of the photosphere, and analyzes the various phases of the eruption. The eruption begins when the ratio of the current to the total mass reaches a critical value beyond which no neighboring equilibrium exists. The height at which the prominence erupts depends on twist, and is typically comparable with the footpoint half-separation. Emphasis is placed on the role of the external field reconnection below the filament, as well as that the mass loss through the legs in the early phases of the eruption.

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