Authors: Federico Fraternale (Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntville)

The interaction of the solar wind with the local interstellar medium, which creates the heliosphere, is complex as it involves an extremely broad range of spatial and temporal scales, and multicomponent, partialy ionized, magnetized plasmas.  Turbulence is ubiquitous in all heliospheric regions and in the local interstellar medium. Global models of the heliosphere describe the time-dependent SW-LISM interaction and large scale structures and can incorporate turbulence transport models. However, it is computationally infeasible to resolve all the relevant scales. Besides, turbulence models applicable to the inner and outer heliosheath, where turbulence becomes compressible and pickup ions energetically dominant, need to be developed. Focusing on the outer heliosphere, this presentation discusses the large-scale heliospheric structures, evidence and properties of turbulence, its potential role in global heliosphere shape, and the current challenges to model the turbulent SW-LISM interaction globally.