Abstract This report gives a summary of the principal properties of coronal transients or coronal mass ejections (CMEs) from the view-point of magnetic field energy transport through the solar corona. The origin of a coronal streamer system is discussed in the context of a large-scale magnetic field configuration pre-existing to transients and mass ejections. Magnetic reconnection driven by the solar wind is highlighted for its non-steady character as well as for its key role in the global dynamics of plasma flows in the corona. The interaction between streamers seems to be important for understanding the nature of CMEs and associated flares. Finally, several remaining issues are stated to be answered with future observations and theoretical works.
Magnetically driven coronal transients
Advances in Space Research ; 11 , 1 ; 179-185
1991-01-01
7 pages
Article (Journal)
Electronic Resource
English
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