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Magnetohydrodynamic simulation of a solar flare: 2. Flare model and simulation using active-region magnetic maps

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Abstract

The results of a three-dimensional MHD simulation and data obtained using specialized spacecraft made it possible to construct an electrodynamic model of solar flares. A flare results from explosive magnetic reconnection in a current sheet above an active region, and electrons accelerated in field-aligned currents cause hard X rays on the solar surface. In this review, we considered works where the boundary and initial conditions on the photosphere were specified directly from the magnetic maps, obtained by SOHO MDI in the preflare state, in order to simulate the formation of a current sheet. A numerical solution of the complete set of MHD equations, performed using the new-generation PERESVET program, demonstrated the formation of several current sheets before a series of flares. A comparison of the observed relativistic proton spectra and the simulated proton acceleration along a magnetic field singular line made it possible to estimate the magnetic reconnection rate during a flare (∼107 cm s−1). Great flares (of the X class) originate after an increase in the active region magnetic flux up to 1022 Mx.

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Authors and Affiliations

  1. Lebedev Physical Institute, Russian Academy of Sciences, Leninskii pr. 53, Moscow, 119991, Russia

    A. I. Podgorny

  2. Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya ul. 48, Moscow, 109017, Russia

    I. M. Podgorny

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  1. A. I. Podgorny
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  2. I. M. Podgorny
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Correspondence to A. I. Podgorny.

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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. 176–189.

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Podgorny, A.I., Podgorny, I.M. Magnetohydrodynamic simulation of a solar flare: 2. Flare model and simulation using active-region magnetic maps. Geomagn. Aeron. 52, 162–175 (2012). https://doi.org/10.1134/S0016793212020119

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  • DOI: https://doi.org/10.1134/S0016793212020119

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