Magnetic reconnection as a mechanism for heating the persistent coronal loops

Abstract

A simplified self-consistent model is applied to determine the parameters describing a steady, high-temperature turbulent current sheet subject to a small transverse magnetic field component as well as anomalous electrical and thermal conductivity. Magnetic reconnection in such a sheet might serve as the energy source and drive the plasma flows observed in slow coronal transients, the long-lived loops that persist in the solar corona for tens of hours.