Three-Dimensional Structure of Solar Wind Turbulence

Details Three-Dimensional Structure of Solar Wind Turbulence Three-Dimensional Structure of Solar Wind Turbulence

2011-09-12

arxiv.org/abs/1109.2558v1

Physics

Space Physics

Scientific paper

We have measured, for the first time, the three-dimensional structure of inertial range plasma turbulence in the fast solar wind with respect to a local, physically motivated coordinate system. We found that the incompressible Alfvenic fluctuations are three-dimensionally anisotropic, with the sense of this anisotropy changing from large to small scales. At the largest scales, the magnetic field correlations are longest in the local fluctuation direction, consistent with Alfven waves. At the smallest scales, they are longest along the local mean field direction and shortest in the direction perpendicular to the local mean field and the local field fluctuation. The compressive fluctuations are highly elongated along the local mean magnetic field direction, although axially symmetric perpendicular to it. Their large anisotropy may explain why they are not heavily damped.

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