  Solar wind measurements carried out by NASA's Wind spacecraft before, during
and after the passing of an interplanetary coronal mass ejection (ICME)
detected on 12-14 September 2014 have been used in order to examine several
properties of magnetohydrodynamic (MHD) turbulence. Spectral indices and
flatness scaling exponents of magnetic field, velocity and proton density
measurements were obtained, and provided a standard description of the
characteristics of turbulence within different sub-regions of the ICME and its
surroundings. This analysis was followed by the validation of the third-order
moment scaling law for isotropic, incompressible MHD turbulence in the same
sub-regions, which confirmed the fully developed nature of turbulence in the
ICME plasma. The energy transfer rate was also estimated in each ICME
sub-region and in the surrounding solar wind. An exceptionally high value was
found within the ICME sheath, accompanied by enhanced intermittency, possibly
related to the powerful energy injection associated with the arrival of the
ICME.
