Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh51c..02p&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH51C-02
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7519 Flares, 7524 Magnetic Fields, 7526 Magnetic Reconnection (2723, 7835)
Scientific paper
The most violent solar coronal phenomena all involve magnetic reconnection which allows the release of stored magnetic energy into other forms of energy. The triggering of solar reconnection in a low resistivity environment requires the build-up of intense electric current sheets, which are also the cornerstone of particle acceleration mechanisms. Magnetic configurations with a complex topology, i.e., with separatrices, are the most obvious configurations where current sheets can form, and therefore where reconnection can efficiently occur. As I will show through several examples, motions of the field lines at the photospheric level, even if regular, slow and spatially smooth, can lead to the formation of current sheets along the separatrices. However, with such topology the formation of the current sheet is extremely fast, so there is little time for energy to build up before reconnection sets in. How can large amounts of magnetic energy be stored before reconnection is triggered? "Quasi-Separatrix Layers" (QSLs), which are regions where there is a drastic yet continuous change in field-line linkage, generalizing the definition of separatrices, offer a natural solution to this storage problem. Based on observational and numerical examples, I will compare the energy build-up problem in separatrices and QSLs topologies and discuss the implications on the observable properties of reconnection.
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