Abstract
The results of modeling the preflare situation in the solar corona, obtained using a numerical solution for a complete set of three-dimensional MHD equations, are reviewed. Any assumptions concerning the flare development character or the active region’s behavior before a flare are not introduced. The initial and boundary conditions on the photosphere are specified from magnetic field measurements before a flare. The photospheric field sources are approximated by magnetic dipoles. The usage of the PERESVET program indicated that a current sheet is formed in the vicinity of a singular magnetic field line in the corona. The sheet is formed due to disturbances coming from the photosphere. The energy necessary for a flare is stored in the current sheet magnetic field during 2–3 days. The main construction principles of the PERESVET program, which makes it possible to use the maps of a measured photospheric field as boundary conditions, are presented.
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Original Russian Text © A.I. Podgorny, I.M. Podgorny, 2012, published in Geomagnetizm i Aeronomiya, 2012, Vol. 52, No. 2, pp. 163–175.
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Podgorny, A.I., Podgorny, I.M. Magnetohydrodynamic simulation of a solar flare: 1. Current sheet in the corona. Geomagn. Aeron. 52, 150–161 (2012). https://doi.org/10.1134/S0016793212020107
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DOI: https://doi.org/10.1134/S0016793212020107