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Quasistationary phenomena in the solar corona

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Postflare loops, which fill by hot plasma from chromospheric sources, are numerically simulated. The PERESVET code is used to solve the system of resistive magnetohydrodynamic equations. The possible mechanisms of plasma heating in the loop are discussed. It is shown that plasma heating can be produced by magnetic line reconnection. The stable plasma confinement in the arch magnetic field of the solar corona is determined by field-aligned current generation.
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Keywords: Sun; post-flare loops; solar corona

Document Type: Research Article

Affiliations: 1: Institute for Astronomy Russian Academy of Science Moscow 109017 Russia 2: P.N. Lebedev Physical Institute Russian Academy of Science Moscow 119991 Russia 3: Osaka City University Osaka 558 Japan

Publication date: 2003-08-01

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