Anisotropic Cascades in Interstellar Medium Turbulence

Details Anisotropic Cascades in Interstellar Medium Turbulence Anisotropic Cascades in Interstellar Medium Turbulence

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007apj...656l..17s&link_type=abstract

The Astrophysical Journal, Volume 656, Issue 1, pp. L17-L20.

Astronomy and Astrophysics

Astronomy

15

Interplanetary Medium, Ism: Kinematics And Dynamics, Methods: Numerical, Magnetohydrodynamics: Mhd, Sun: Solar Wind, Turbulence

Scientific paper

Anisotropic turbulent cascades in the solar wind and interstellar medium (ISM) are investigated using three-dimensional incompressible magnetohydrodynamic (MHD) simulations with a numerical resolution of 2563. In the absence of an external magnetic field (B0=0), the anisotropy in the MHD turbulent fluctuations is mediated primarily by the local magnetic field. The latter leads to a disparity in the spectral transfer of energy along and across the local mean magnetic field. While the anisotropic cascades give rise to the relationship λ˜∥~λ˜2/3⊥ between the parallel (λ˜∥~1/k∥) and perpendicular (λ˜⊥~1/k⊥) length scales of the eddies relative to the local magnetic field, the global energy is found to obey a Kolmogorov-like k-5/3 anisotropic spectrum in our simulations where turbulence is predominantly subcritical. In the latter, the turbulent cascades are dominated by the nonlinear eddy turnover timescales compared to the linear Alfvén wave periods. The critical-balance criterion is therefore not necessarily satisfied in fully developed, strong, anisotropic, high plasma-β magnetofluid ISM turbulence.

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