Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh12b0754l&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SH12B-0754
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7513 Coronal Mass Ejections, 7519 Flares, 7524 Magnetic Fields, 7529 Photosphere
Scientific paper
Theoretical and observational works (Lin and Forbes, 2000; Forbes and Lin, 2000; Akmal et al., 2001) indicate the existence of an extensive current sheet below the plasmoid ejected by a major eruption, such as two-ribbon flare, eruptive prominence, as well as coronal mass ejection (CME). This current sheet, together with the field lines connected to it which is known as separatrix, obviously distinguishes two magnetic flux systems that have different topological connections. Extending to three-dimensional configurations, they become separatrix surface (Démoulin et al., 1993) and quasi-separatrix layers (Priest and Démoulin, 1995). These terms imply that activities or eruptons occur around the surface or the layer. On the other hand, both theories and observations also show that it is not necessary for all of the surfaces or layers which separate two different topological connection magnetic fluxes to be the precursors of eruptions although the likelyhood of eruptions can be very high. To generalize the concept, Wang (1998) and Wang (1999) suggested to use the term of "magnetic interface" to describe such a surface or layer in the coronal that separates two or more magnetic flux systems which do not topologically connect. The electric conductivity of the coronal plasma is fairly high although it is not infinitely high, the dissipation of the magnetic field is generally very slow in the region without neutral point, so the magnetic fluxes with different topological connections can survive for a quite while. This is the base for the concept of the magnetic interface. However, the coronal magnetic field evolves in response to the change in the photospheric field because the coronal field is line-tied to the photosphere. This implies that the magnetic interface, if exists, has to evolves simultaneously. In the present work, we are going to specify the concept clearly on the base of current CME models. We will show how an 3D interface evolves to a current sheet and separatrix surface, and will also show how an interface survives during evolution without evovling to the current sheet or separatrix. We found that the introduction of the magnetic interface is quite useful for identifying prospective active regions and for forecasting the energetic activities.
Lin Juhn-Jong
van Ballegooijen Adriaan A.
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