Abstract
A short review is given about the self‐consistent MHD model of solar coronal heating recently proposed by Bigot et al. (2008) in which the dynamical effect of the background magnetic field along a coronal structure is taken into account through exact results from Alfvén wave turbulence. The main properties of the model are given as well as the heating rate and the microturbulent velocity obtained in the case of coronal loops. The conclusion is that Alfvén wave turbulence may produce an efficient background heating for the solar corona.
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