Anisotropy of Alfvénic Turbulence in the Solar Wind and Numerical Simulations

Details Anisotropy of Alfvénic Turbulence in the Solar Wind and Numerical Simulations Anisotropy of Alfvénic Turbulence in the Solar Wind and Numerical Simulations

2010-09-03

arxiv.org/abs/1009.0662v2

Mon. Not. Roy. Astron. Soc. 415: 3219,2011

Physics

Space Physics

9 pages, 8 figures

Scientific paper

10.1111/j.1365-2966.2011.18933.x

We investigate the anisotropy of Alfv\'enic turbulence in the inertial range of slow solar wind and in both driven and decaying reduced magnetohydrodynamic simulations. A direct comparison is made by measuring the anisotropic second-order structure functions in both data sets. In the solar wind, the perpendicular spectral index of the magnetic field is close to -5/3. In the forced simulation, it is close to -5/3 for the velocity and -3/2 for the magnetic field. In the decaying simulation, it is -5/3 for both fields. The spectral index becomes steeper at small angles to the local magnetic field direction in all cases. We also show that when using the global rather than local mean field, the anisotropic scaling of the simulations cannot always be properly measured.

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