Is the CME magnetic energy stored in coronal flux ropes ?

Details Is the CME magnetic energy stored in coronal flux ropes ? Is the CME magnetic energy stored in coronal flux ropes ?

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41c06a&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH41C-06 INVITED

Physics

7513 Coronal Mass Ejections, 7524 Magnetic Fields, 7531 Prominence Eruptions

Scientific paper

MHD theory, coronograph and in situ solar wind observations are consistent with a flux rope like topology for many CME's. However, this does not permit to conclude that the pre-eruptive coronal magnetic field does have this topology. This is because any erupting fields must lead to the formation of a vertical current sheet, in which reconnection can form the so-called coronal postflare loops, as well as a large flux rope which surrounds the erupting fields, which are ejected alltogether. The only physical property of the pre-eruptive fields which is required for triggering a CME is that they must be ``stressed'', i.e. they must contain strong electric currents. As prominences are the largest and best observed stressed magnetic configurations of the solar atmosphere, and as they often lead to CME's, they provide a unique opportunity for studying the pre-CME magnetic field topology. Based on a compilation of old and recent results, I will show that both magnetic and multi-wavelength observations strongly support a uniform flux rope like topology for prominences. Then, I will compare the predicted flux/twist/helicity with the values measured in interplanetary magnetic clouds, and I will discuss the role of the large scale fields for the development of CME's. I will end on possible theoretical and observational prospectives which should be achieved for the study of stressed fields in prominences and in active regions (e.g. delta-spots).

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