Heating of coronal loops: weak MHD turbulence and scaling laws

To understand the nonlinear dynamics of the Parker scenario for coronal heating, longtime high-resolution simulations of the dynamics of a coronal loop in cartesian geometry are carried out. A loop is modeled as a box extended along the direction of the strong magnetic field B-0 in which the system is embedded. At the top and bottom plates, which represent the photosphere, velocity fields mimicking photospheric motions are imposed. We show that the nonlinear dynamics is described by different regimes of MHD anisotropic turbulence, with spectra characterized by intertial range power laws whose indexes range from Kolmogorov-like values (similar to 5/3) up to similar to 3. We briefly describe the beating for coronal heating rates.