  Low frequency turbulence in Saturn's magnetosheath is investigated using
in-situ measurements of the Cassini spacecraft. Focus is put on the magnetic
energy spectra computed in the frequency range $\sim[10^{-4}, 1]$Hz. A set of
42 time intervals in the magnetosheath were analyzed and three main results
that contrast with known features of solar wind turbulence are reported: 1) The
magnetic energy spectra showed a $\sim f^{-1}$ scaling at MHD scales followed
by an $\sim f^{-2.6}$ scaling at the sub-ion scales without forming the
so-called inertial range; 2) The magnetic compressibility and the
cross-correlation between the parallel component of the magnetic field and
density fluctuations $ C(\delta n,\delta B_{||}) $ indicates the dominance of
the compressible magnetosonic slow-like modes at MHD scales rather than the
Alfv\'en mode; 3) Higher order statistics revealed a monofractal (resp.
multifractal) behaviour of the turbulent flow downstream of a
quasi-perpendicular (resp. quasi-parallel) shock at the sub-ion scales.
Implications of these results on theoretical modeling of space plasma
turbulence are discussed.
