Solar flare model: Comparison of the results of numerical simulations and observations

Details Solar flare model: Comparison of the results of numerical simulations and observations Solar flare model: Comparison of the results of numerical simulations and observations

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ge%26ae..49.1115p&link_type=abstract

Geomagnetism and Aeronomy, Volume 49, Issue 8, pp.1115-1119

Computer Science

Scientific paper

The electrodynamic flare model is based on numerical 3D simulations with the real magnetic field of an active region. An energy of ˜1032 erg necessary for a solar flare is shown to accumulate in the magnetic field of a coronal current sheet. The thermal X-ray source in the corona results from plasma heating in the current sheet upon reconnection. The hard X-ray sources are located on the solar surface at the loop foot-points. They are produced by the precipitation of electron beams accelerated in field-aligned currents. Solar cosmic rays appear upon acceleration in the electric field along a singular magnetic X-type line. The generation mechanism of the delayed cosmic-ray component is also discussed.

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