Magnetosheath Turbulence

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2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma, 2724 Magnetopause And Boundary Layers, 2728 Magnetosheath, 4455 Nonlinear Waves, Shock Waves, Solitons (0689, 2487, 3280, 3285, 4275, 6934, 7851, 7852)

Scientific paper

The Earth's magnetosheath is a transition region between the solar wind and the magnetosphere. An important question is how does the solar wind turbulence change across the bow-shock? The bow shock introduces an important temperature anisotropy. Relaxation of this anisotropy is accompanied by the generation Alfvén Ion Cyclotron (AIC) and mirror linear waves at frequencies below the ions cyclotron frequency fci. The superposition of these waves gives the spectrum of magnetic fluctuations ~ f- 1 in the vicinity of the bow-shock. In the flanks, however, we observe, for the first time, the Kolmorogov's ~ f-5/3 spectrum. At higher frequencies, f>fci, as in the solar wind, turbulent spectrum follows a ~ f-3 power law. At the difference with the solar wind turbulence, the transition between one inertial range to another is often accompanied by the presence of Alfvén vortices at the spectral break scales. Recent observations in the Kronian magnetosheath show the presence of such vortices at the same scales, revealing the generality of the phenomena. Alfvén vortex is a non-linear Alfvén wave with wavevectors k mainly perpendicular to a mean field. We show that this anisotropy of a turbulent energy distribution in k--space, i.e. k⊥≫ k|, is observed not only within the vortices, but for the whole range of small scales above the spectral break. This is observed for different plasma beta β in [1,10] and independently on the presence of the AIC or mirror waves at larger scales. We discuss possible influence of the magnetosheath turbulence features on the magnetopause reconnection.

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