Imprints of expansion onto the local anisotropy of solar wind turbulence

Abstract

We study the anisotropy of II-order structure functions defined in a frame attached to the local mean field in three-dimensional (3D) direct numerical simulations of magnetohydrodynamic turbulence, including or not the solar wind expansion. We simulate spacecraft flybys through the numerical domain by taking increments along the radial (wind) direction that forms an angle of $45^o$ with the ambient magnetic field. We find that only when expansion is taken into account, do the synthetic observations match the 3D anisotropy observed in the solar wind, including the change of anisotropy with scales. Our simulations also show that the anisotropy changes dramatically when considering increments oblique to the radial directions. Both results can be understood by noting that expansion reduces the radial component of the magnetic field at all scales, thus confining fluctuations in the plane perpendicular to the radial. Expansion is thus shown to affect not only the (global) spectral anisotropy, but also the local anisotropy of second-order structure functions by influencing the distribution of the local mean field, which enters this higher-order statistics.

5 pages, 5 figures, accepted in ApJL

References in corpus (5)

• Comparison of spectral slopes of magnetohydrodynamic and hydrodynamic turbulence and measurements of alignment effects
• Anisotropy of third-order structure functions in MHD turbulence
• Evolution of turbulence in the expanding solar wind, a numerical study
• Measuring the Alfvenic Nature of the Interstellar Medium: Velocity Anisotropy Revisited
• Correlations at large scales and the onset of turbulence in the fast solar wind

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