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The nature of subproton scale fluctuations in the solar wind is an openquestion, partly because two similar types of electromagnetic turbulence canoccur: kinetic Alfven turbulence and whistler turbulence. These twopossibilities, however, have one key qualitative difference: whistlerturbulence, unlike kinetic Alfven turbulence, has negligible power in densityfluctuations. In this Letter, we present new observational data, as well asanalytical and numerical results, to investigate this difference. The resultsshow, for the first time, that the fluctuations well below the proton scale arepredominantly kinetic Alfven turbulence, and, if present at all, the whistlerfluctuations make up only a small fraction of the total energy.

The Nature of Subproton Scale Turbulence in the Solar Wind