TURBULENT CORONAL HEATING .1. SHEARED ARCADE

The model of Heyvaerts & Priest (1992) for heating the solar corona by turbulent processes in a sheared arcade is examined in more detail by numerically solving their basic equations for the turbulent viscosity , magnetic diffusivity, velocity and energy flux density. A weighted s pectrum for the mean square velocity in the photosphere and a scale-de pendent turbulent viscosity and magnetic diffusivity for local eddy re laxation are introduced which improve the self-consistency of the mode l. Estimates are made of the turbulent variables listed above which ar e found to accord well with the requirements for heating a solar activ e region (approximate to 10(7) erg cm(-2) s(-1)).