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In the solar wind, power spectral density (PSD) of the magnetic fieldfluctuations generally follow the so-called Kolmogorov spectrum f^-5/3 in theinertial range, where the dynamics is thought to be dominated by nonlinearinteractions between counter-propagating incompressible Alfv\'en wave parquets.These features are thought to be ubiquitous in space plasmas. The present studygives a new and more complex picture of magnetohydrodynamics (MHD) turbulenceas observed in the terrestrial magnetosheath. The study uses three years ofin-situ data from the Cluster mission to explore the nature of the magneticfluctuations at MHD scales in different locations within the magnetosheath,including flanks and subsolar regions. It is found that the magnetic fieldfluctuations at MHD scales generally have a PSD close to f^-1 (shallower thanthe Kolmogorov one f^-5/3) down to the ion characteristic scale, which recallsthe energy containing scales of solar wind turbulence. The Kolmogorov spectrumis observed only away from the bow shock toward the flank and the magnetopauseregions in 17% of the analyzed time intervals. Measuring the magneticcompressibility, it is shown that only a fraction (35%) of the observedKolmogorov spectra were populated by shear Alfv\'enic fluctuations, whereas themajority of the events (65%) was found to be dominated by compressiblemagnetosonic-like fluctuations, which contrasts with well-known turbulenceproperties in the solar wind. This study gives a first comprehensive view ofthe origin of the f^-1 and the transition to the Kolmogorov inertial range;both questions remain controversial in solar wind turbulence.

On the Existence of the Kolmogorov Inertial Range in the Terrestrial Magnetosheath Turbulence