Multi-scale Numerical Approach to Solar Flare Magnetic Reconnection

Details Multi-scale Numerical Approach to Solar Flare Magnetic Reconnection Multi-scale Numerical Approach to Solar Flare Magnetic Reconnection

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.3.49b&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

Magnetic reconnection - considered now commonly as the engine of solar flares - spans over many mutually coupled scales from the global flare dimensions (approximately 10 Mm) down to the scale, where dissipation through kinetic effects take place (approximately 10 m). Direct numerical simulation covering all the scales is therefore impossible for obvious reasons: full 3D numerical model would have to involve 1018 grid points. Nevertheless, the filamentary nature of the current sheet fragmentation give us the chance to describe the process of reconnection with highly reduced request for number of grid points. As the smaller-scale dynamics is interesting only in regions of enhanced current sheet filamentation, we can focus just on these areas, which occupy only a small fraction of the total volume. Generally, as the fragmentation continues, it forms a cascade (finished by the kinetic dissipation) where information relevant for description of the smaller-scale level occupies only a small fraction of grid points describing the higher level. Thus, one can subsequently zoom-in onto the regions of continuing current filamentation. Anticipated current-sheet-fragmentation cascade supposes multiple dissipative regions formed in a single current sheet - this fact can play a key role for direct particle acceleration in reconnection. The numerical algorithm implementing this 'zooming' technique and the first results will be presented.

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