On the formation of coronal cavities

Details On the formation of coronal cavities On the formation of coronal cavities

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph..102..165a&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 102, no. 1-2, Dec. 1985, p. 165-176. NASA-supported research.

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Coronal Holes, Plasma Dynamics, Solar Activity, Solar Prominences, Cavities, Computational Fluid Dynamics, Field Strength, Solar Magnetic Field, Solar Wind

Scientific paper

The formation of a coronal cavity and its relation to a quiescent prominence is studied theoretically. The stability of condensation modes of a plasma in the coronal streamer model (Steinolfson et al., 1982) is considered using a two-dimensional time-dependent ideal MHD numerical simulation. It is found that a plasma with beta = 0.5 is unstable but one with beta = 4 is stable because the density enhancement of the plasma trapped by the closed fields increases with the strength of the magnetic field. The means by which condensation modes can produce a coronal cavity and/or initiate the formation of a prominence (depending on the field configuration) are discussed. It is argued that prominence and cavity material is all supplied from the chromospheric level in the form of spicules.

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