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 magneticfield is simulated using the data from the photospheric magnetic fieldmeasurements. The distinctive feature of the new model is incorporating the MHDAlfven wave turbulence. We assume this turbulence and its non-lineardissipation to be the only momentum and energy source for heating the coronalplasma and driving the solar wind. The difference between the turbulencedissipation efficiency in coronal holes and that in closed field regions isbecause the non-linear cascade rate degrades in strongly anisotropic turbulencein coronal holes (no inward propagating wave), thus resulting in colder coronalholes with the bi-modal solar wind originating from them. The detailedpresentation of the theoretical model is illustrated with the synthetic imagesfor multi-wavelength EUV emission compared with the observations from SDO AIAand Stereo EUVI instruments for the Carrington rotation 2107.
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