Search

Plasma turbulence at ion kinetic scales in the solar wind is investigated using the multi-point magnetometer data from the Cluster spacecraft. By applying the k-filtering method, we are able to estimate the full three-dimensional power spectral density P(?sc, k) at a certain spacecraft frequency ?sc in wavevector (k) space. By using the wavevector at the maximum power in P(?sc, k) at each sampling frequency ?sc and the Doppler shifted frequency ?pla in the solar wind frame, the dispersion plot ?pla = ?pla(k) is found. Previous studies have been limited to very few intervals and have been hampered by large errors, which motivates a statistical study of 52 intervals of solar wind. We find that the turbulence is predominantly highly oblique to the magnetic field k ? k ?, and propagates slowly in the plasma frame with most points having frequencies smaller than the proton gyrofrequency ?pla < ? p . Weak agreement is found that turbulence at the ion kinetic scales consists of kinetic Alfv?n waves and coherent structures advected with plasma bulk velocity plus some minor more compressible components. The results suggest that anti-sunward and sunward propagating magnetic fluctuations are of similar nature in both the fast and slow solar wind at ion kinetic scales. The fast wind has significantly more anti-sunward flux than sunward flux and the slow wind appears to be more balanced.

The k-filtering technique and wave polarization analysis are applied to Cluster magnetic field data to study plasma turbulence at the scale of the ion gyroradius in the fast solar wind. Waves are found propagating in directions nearly perpendicular to the background magnetic field at such scales. The frequencies of these waves in the solar wind frame are much smaller than the proton gyro-frequency. After the wave vector ${\bf k}$ is determined at each spacecraft frequency $f_{sc}$, wave polarization property is analyzed in the plane perpendicular to ${\bf k}$. Magnetic fluctuations have $\delta B_\perp>\delta B_\parallel$ (here the $\parallel$ and $\perp$ refer to the background magnetic field ${\bf B}_0$). The wave magnetic field has right-handed polarization at propagation angles $\theta_{\bf kB}90^\circ$. The magnetic field in the plane perpendicular to ${\bf B}_0$ however has no clear sense of a dominant polarization but local rotations. We discuss the merits and limitations of linear kinetic Aflv\'en waves (KAWs) and coherent Alfv\'en vortices in the interpretation of the data. We suggest that the fast solar wind turbulence may be populated with KAWs, small scale current sheets and Alfv\'en vortices at ion kinetic scales., Comment: 6 pages, 5 figures, Accepted by ApJ