Intermittency in MHD turbulence: Solar wind observations and coronal nanoflares modelling

High resolution numerical simulations, solar wind data analysis, and measurements at the edges of laboratory plasma devices have allowed for a huge progress in our understanding of MHD Turbulence. In particular the high resolution of solar wind measurements has allowed to characterize the intermittency observed at small scales. We are now able to set up a consistent and convincing view of the main properties of MHD turbulence, which in turn constitutes an extremely efficient tool in understanding the behavior of turbulent plasmas, like those in solar corona, where in situ observations are not available. In particular, using this knowledge a model to describe the turbulence generated by footpoint motions in a coronal loop has been built up, which has allowed for a detailed comparison between statistical properties of intermittent dissipative events in the loop and nanoflare observations.