TURBULENT CORONAL HEATING .3. WAVE HEATING IN CORONAL LOOPS

The heating which results from damped oscillations of a uniform solar coronal loop driven by photospheric motions is considered for an incom pressible, visco-resistive, turbulent medium. Photospheric disturbance s on a time-scale faster than the time for an Alfven wave to cross the loop drive damped standing waves in the loop. Including turbulent eff ects permits the generation of gradients sufficiently intense to allow dissipation of the kinetic and magnetic energy of the waves to balanc e the rate of injection of energy from the photosphere, thus maintaini ng a steady state. Assuming a single global driving frequency, levels of heating approaching 10(4) Wm(-2) (10(7) erg cm(-2) s(-1)) are attai nable for the fundamental resonance and first few harmonics, which cou ld account for the heating of short (10(4) km) loops with fields of or der 100 G if sufficiently rapid photospheric oscillations occur. Also, for fields of about 10G, which occur in the longer loops (10(5) km) f ound outside active regions, levels approaching 100 Wm(-2) (10(5) erg cm(-2) s(-1)) are obtained - sufficient to heat the quiet corona.