Turbulent MHD waves have been traditionally considered as a possible energy source for coronal heating and solar wind acceleration. Here we present a newly developed computational model in which the self-consistent system of the wave transport equation coupled with the MHD equations is solved. The model is four-dimensional (three spatial coordinates plus wave frequency). The inner boundary condition for the Alfvén waves energy flux is determined for each point on the solar surface and is related to the magnetogram structure.