Physics
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.3.34p&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
By numerical solving of the 3D MHD equations system it is shown several current sheets appearance before the set of flares. Each sheet can produce an elementary flare. Several current sheets creation influence on the general field configuration above the active region can be essential. X-points positions found in the potential magnetic field can strongly differ from positions of created current sheets. For the MHD simulation of flare situation in the corona all conditions are taken from observed magnetic field distributions on the photosphere. SOHO MDI maps are used. For initial conditions setting the method of numerical Laplace equation solving with inclined derivative as the boundary condition is developed. The initial magnetic field above the active region is potential one. It is calculated before new magnetic flux emergence. To stabilize the numerical instabilities a number of numerical methods are developed and programming realized in the PERESVET code. The finite-difference scheme for MHD equations is absolutely implicit, and it is conservative relative to the magnetic flux. Behavior of divB in the time evolution is described by diffusion equation. Calculations for active regions with different sizes show, that for finding of the real magnetic field in the corona it is necessary to perform simulations in a large region with the size order of 5x10^{10} cm. The sheets appeared near the emerged X-points are almost vertical ones. So the flares in these sheets can produce CME, because the jxB force, which accelerates plasma in the sheet, is directed away from the Sun. The typical time of magnetic energy accumulation for a flare is several tens hours. During this time the magnetic North and South fluxes through an active region increase in 1e21 - 1e22 Mx.
Podgorny A.
Podgorny I.
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