future paper. Finally, we do not address the more realistic case of a single photosphere with curved coronal loops, such as the simulations presented recently by @gud05. While this approach has advantages when investigating the coronal loop dynamics within its coronal neighborhood, modeling a larger part of the solar corona numerically drastically reduces the number of points occupied by the coronal loops. At the moment the very low resolution attainable with this kind of simulations does not allow the development of turbulence with a well-developed inertial range. The transfer of energy from the scale of convection cells $\sim 1000\, km$ toward smaller scales is inhibited, because the smaller scales are not resolved (their linear resolution is $\sim 500\, km$). Thus, these simulations have not been able to shed light on the detailed coronal statistical response nor on the different regimes which may develop and how they depend on the coronal magnetic field crossing time and the photospheric eddy turnover time.

In § \[sec:model\] we introduce the coronal loop model, whose properties are qualitatively analyzed in § \[sec:an\]. The results of our simulations are described in § \[sec:ns\], and their turbulence properties are analyze in more detail in § \[sec:wts\]. Finally 