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Astron. Astrophys. 354, 703-713 (2000)

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Slow and fast magnetic reconnection

II. High-temperature turbulent-current sheet

B.V. Somov and A.V. Oreshina

Solar Physics Department, Astronomical Institute, Moscow State University, Universitetskii Prospekt 13, Moscow 119899, Russian Federation (somov@sai.msu.su)

Received 27 July 1999 / Accepted 20 October 1999

Abstract

 We present a new magnetohydrodynamic model of high-temperature ([FORMULA]) turbulent-current sheet forming in regions of magnetic reconnection in the solar corona. A structure of the sheet is studied with allowance for such effects as anomalous resistivity of plasma, radiative cooling, anomalous heat conduction. The relative roles of the two latter factors in the current sheet energy balance are shown. The model describes both the slow regime of reconnection (with O-type magnetic configuration in the center of the sheet) and the fast one (with X-type configuration). Energy release power in the current sheet at the fast regime of reconnection is sufficient to account for solar flares and coronal transients.

Key words: Magnetohydrodynamics (MHD) – Sun: corona – Sun: flares – Sun: magnetic fields

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© European Southern Observatory (ESO) 2000

Online publication: February 9, 2000
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