Physics
Scientific paper
Mar 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..119..157s&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 119, no. 1, 1989, p. 157-195. Research supported by SERC.
Physics
25
Magnetic Field Reconnection, Solar Corona, Solar Magnetic Field, Solar Prominences, Stellar Mass Ejection, Coronal Loops, Magnetohydrodynamics, Mathematical Models
Scientific paper
Two possible limiting scenarios for the production of a coronal mass ejection are considered: (1) the magnetic field around a prominence evolving until it loses equilibrium and erupts, driving reconnection below the prominence and the eruption of the overlying magnetic arcade; and (2) a large-scale magnetic arcade evolving until it loses equilibrium and erupts, causing a prominence to erupt. A model for the eruption of a magnetically coupled prominence and coronal mass ejection is proposed which overcomes several of the limitations of the model of Anzer and Pneuman (1982). For all the cases investigated, the prominence and mass ejection are found to accelerate upward before reaching constant velocities, in a manner which is consistent with observations.
Priest Eric R.
Steele Colin D. C.
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