  Turbulence properties are examined before, during and after a coronal mass
ejection (CME) detected by the6Wind spacecraft on July 2012. The power-law
scaling of the structure functions, providing information on the7power spectral
density and flatness of the velocity, magnetic filed and density fluctuations,
were examined. The8third-order moment scaling law for incompressible, isotropic
magnetohydrodynamic turbulence was observed9in the preceding and trailing solar
wind, as well as in the CME sheath and magnetic cloud. This suggests that10the
turbulence could develop sufficiently after the shock, or that turbulence in
the sheath and cloud regions11was robustly preserved even during the mixing
with the solar wind plasma. The turbulent energy transfer rate12was thus
evaluated in each of the regions. The CME sheath shows an increase of energy
transfer rate, as13expected from the lower level of Alfv\'enic fluctuations and
suggesting the role of the shock-wind interaction as14an additional source of
energy for the turbulent cascade.
