Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 415, Issue 4, Pages 3219-3226Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2011.18933.x
Keywords
magnetic fields; MHD; plasmas; turbulence; solar wind
Categories
Funding
- STFC
- Leverhulme Trust Network for Magnetized Plasma Turbulence
- STFC [ST/F002505/2, ST/I002138/1] Funding Source: UKRI
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We investigate the anisotropy of Alfvenic 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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