Coronal MHD transport theory and phenomenology

In the presence of a weakly inhomogeneous background, magnetohydrodynamic fluctuations are transported, reflected and at small scales, dissipated. In contrast to orderings appropriate to outer solar wind conditions, here we explore transport in a regime relevant for solar coronal heating and solar wind acceleration, in which effects of the order of the Alfven speed are retained while disregarding the solar wind velocity. We consider the general properties of the transport equations as well as some solutions of interest.