Solar wind turbulence at kinetic scales

International audienceSolar wind is a turbulent magnetized collisionless plasma. Kolmogorov's turbulent spectrum is widely observed at magnetohydrodynamic scales. At smaller scales, i.e. at scales of the order of the kinetic plasma scales (such as Larmor radii of charged particles or their inertial lengths, ~ 50 km for protons and ~ 2 km for electrons), turbulence is less studied and is a matter of debate. In this presentation we review different observations related to kinetic range, such as magnetic spectra, signatures of multi- and mono-fractality, wave vector anisotropy and indications of different wave modes. Then, we will show new results related to intermittency and coherent structures present within this range