  Observations reveal nearly power-law spectra of magnetic and density plasma
fluctuations at subproton scales in the solar wind, which indicates the
presence of a turbulent cascade. We discuss the three-field and two-field
models for micro-scale plasma fluctuations, and then present the results of
numerical simulations of a two-field model of kinetic-Alfven turbulence, which
models plasma motion at sub-proton scales.
