Results on 3-D solar magnetic field, observations and models

Details Results on 3-D solar magnetic field, observations and models Results on 3-D solar magnetic field, observations and models

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jastp..61..101d&link_type=abstract

Journal of Atmospheric and Solar-Terrestrial Physics, Volume 61, Issue 1-2, p. 101-108.

Physics

3

Scientific paper

This review presents some of the new developments in the understanding of coronal magnetic fields in flares and coronal mass ejections. The modelling of the coronal magnetic field based on observed photospheric field permits to understand the location of energy release. Various flare observations are consistent with a model where magnetic reconnection occurs between two magnetic fields of different connectivity. Because magnetic helicity is almost conserved, the stored energy cannot be fully released in confined flares. The corona gets rid of the helicity injected by the convection zone only by ejecting part of the magnetic field. A severe physical constraint (open-field limit) on these ejections has been firmly established for force-free fields. It is, however, possible to open partially the field or to eject a twisted flux-tube keeping the energy of the field behind the open-field limit. New results show that in simply connected fields this happen after a finite time without loss of equilibrium, while in more complex topology a loss of equilibrium can still be present.

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