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2.5-dimensional magnetohydrodynamic (MHD) simulations are performed with highspatial resolution in order to distinguish between competing models of thecoronal heating problem. A single coronal loop powered by Alfv\'{e}n wavesexcited in the photosphere is the target of the present study. The coronalstructure is reproduced in our simulations as a natural consequence of thetransportation and dissipation of Alfv\'{e}n waves. Further, the coronalstructure is maintained as the spatial resolution is changed from 25 to 3 km,although the temperature at the loop top increases with the spatial resolution.The heating mechanisms change gradually across the magnetic canopy at a heightof 4 Mm. Below the magnetic canopy, both the shock and the MHD turbulence aredominant heating processes. Above the magnetic canopy, the shock heating ratereduces to less than 10 % of the total heating rate while the MHD turbulenceprovides significant energy to balance the radiative cooling and thermalconduction loss or gain. The importance of compressibility shown in the presentstudy would significantly impact on the prospects of successful MHD turbulencetheory in the solar chromosphere.

Competition between shock and turbulent heating in coronal loop system