Slow and fast magnetic reconnection II. High-temperature turbulent-current sheet

Abstract

We present a new magnetohydrodynamic model of high-temperature (T 10 8 K) turbulent-current sheet forming in regions of magnetic reconnection in the solar corona. A struc- ture 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 so- lar flares and coronal transients.