Turbulence is an ubiquitous phenomenon that can be observed on a huge range of scales, from galaxy clusters down to micro- and nano-fluidics. It is observed mostly in neutral flows, but also in charged, magnetized flows such as astrophysical plasmas. The study of turbulence requires a multiple approach: theoretical, experimental, based on data analysis and on numerical simulations. All these aspects are exploited here, with particular focus on space and laboratory turbulent plasmas.
Most of the visible matter in the universe is in the state of plasma. Often times, astrophysical plasmas have highly turbulent dynamics, resulting in a large number of interesting processes such as: energy dissipation, particle acceleration, excitation of electromagnetic waves, particle heating, magnetic reconnection, formation of shocks. All these phenomena can be studied in-situ only in space plasma, where instruments on-board scientific space missions can take measurements. Data can be studied using specific diagnostic tools, which allow the validation of theories and models. A substantial use of numerical simulations is also necessary. The study of turbulence in the interplanetary space is therefore of broad interest for the understanding of the dynamics of astrophysical plasmas, but also for its implications on laboratory plasmas and for the Sun-Earth interaction.
The study of space plasmas turbulence is based on three main approaches: the analysis of data provided by the scientific mission; the development of theoretical models and novel data analysis techniques; the use of numerical simulations (massive computational resources are often required; these are provided by large facilities for high performance computing, such as CINECA, or the UNICAL HPCC. Examples are the full characterization of intermittency in solar wind turbulence [Sorriso-Valvo et al. 1999; 2015], and the validation of the theoretical prediction for the scaling law of the energy flux in solar wind turbulence [Sorriso-Valvo et al., 2007].