  We present a new global model of the solar corona, including the low corona,
the transition region and the top of chromosphere. The realistic 3D magnetic
field is simulated using the data from the photospheric magnetic field
measurements. The distinctive feature of the new model is incorporating the MHD
Alfven wave turbulence. We assume this turbulence and its non-linear
dissipation to be the only momentum and energy source for heating the coronal
plasma and driving the solar wind. The difference between the turbulence
dissipation efficiency in coronal holes and that in closed field regions is
because the non-linear cascade rate degrades in strongly anisotropic turbulence
in coronal holes (no inward propagating wave), thus resulting in colder coronal
holes with the bi-modal solar wind originating from them. The detailed
presentation of the theoretical model is illustrated with the synthetic images
for multi-wavelength EUV emission compared with the observations from SDO AIA
and Stereo EUVI instruments for the Carrington rotation 2107.
