  Context : We present a self-consistent model of solar coronal heating,
originally developed by Heyvaert & Priest (1992), in which we include the
dynamical effect of the background magnetic field along a coronal structure by
using exact results from wave MHD turbulence (Galtier et al. 2000). Aims : We
evaluate the heating rate and the microturbulent velocity for comparison with
observations in the quiet corona, active regions and also coronal holes.
Methods :The coronal structures are assumed to be in a turbulent state
maintained by the slow erratic motions of the magnetic footpoints. A
description for the large-scale and the unresolved small-scale dynamics are
given separately. From the latter, we compute exactly (or numerically for
coronal holes) turbulent viscosites that are finally used in the former to
close self-consistently the system and derive the heating flux expression.
Results : We show that the heating rate and the turbulent velocity compare
favorably with coronal observations. Conclusions : Although the Alfven wave
turbulence regime is strongly anisotropic, and could reduce a priori the
heating efficiency, it provides an unexpected satisfactory model of coronal
heating for both magnetic loops and open magnetic field lines.
