  We investigate properties of solar wind-like plasma turbulence using direct
numerical simulations. We analyze the transition from large,
magnetohydrodynamic (MHD) scales to the ion characteristic ones using
two-dimensional hybrid (fluid electrons, kinetic ions) simulations. To capture
and quantify turbulence properties, we apply the Karman-Howarth-Monin (KHM)
equation for compressible Hall MHD (extended by considering the plasma pressure
as a tensor quantity) to the numerical results. The KHM analysis indicates that
the transition from MHD to ion scales (the so called ion break in the power
spectrum) results from a combination of an onset of Hall physics and of an
effective dissipation owing to the pressure-strain energy-exchange channel and
resistivity. We discuss the simulation results in the context of the solar
wind.
