Anisotropies of the Magnetic Field Fluctuations at Kinetic Scales in the Solar Wind: Cluster Observations

Abstract

We present the first statistical study of the anisotropy of the magnetic field turbulence in the solar wind between 1 and 200 Hz, I.e., from proton to sub-electron scales. We consider 93 ten-minute intervals of the Cluster/STAFF measurements. We find that the fluctuations δ {B}_\perp ² are not gyrotropic at a given frequency f, a property already observed at larger scales (\parallel /\perp means parallel/perpendicular to the average magnetic {{\boldsymbol{B}}}₀). This non-gyrotropy gives indications of the angular distribution of the wave vectors {\boldsymbol{k}}: at f< 10 Hz, we find that {k}_\perp \gg {k}_\parallel , mainly in the fast wind; at f > 10 Hz, fluctuations with a non-negligible k _∥ are also present. We then consider the anisotropy ratio δ {B}_\parallel ²/δ {B}_\perp ², which is a measure of the magnetic compressibility of the fluctuations. This ratio, always smaller than 1, increases with f. It reaches a value showing that the fluctuations are more or less isotropic at electron scales, for f≥slant 50 {Hz}. From 1 to 15-20 Hz, there is a strong correlation between the observed compressibility and the one expected for the kinetic Alfvén waves (KAWs), which only depends on the total plasma β. For f> 15{--}20 {Hz}, the observed compressibility is larger than expected for KAWs, and it is stronger in the slow wind: this could be an indication of the presence of a slow-ion acoustic mode of fluctuations, which is more compressive and is favored by the larger values of the electron to proton temperature ratio generally observed in the slow wind.