Slow and fast magnetic reconnection
II. High-temperature turbulent-current sheet
B.V. Somov and
Received 27 July 1999 / Accepted 20 October 1999
We present a new magnetohydrodynamic model of high-temperature () 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