Ansiotropic Turbulent Cascades in the Solar Wind and Interstellar Medium

Details Ansiotropic Turbulent Cascades in the Solar Wind and Interstellar Medium Ansiotropic Turbulent Cascades in the Solar Wind and Interstellar Medium

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh13a0383s&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH13A-0383

Physics

2126 Heliosphere/Interstellar Medium Interactions, 2134 Interplanetary Magnetic Fields, 2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma

Scientific paper

Anisotropic turbulent cascades in the solar wind (SW) and interstellar medium (ISM) are investigated using three dimensional incompressible magnetohydrodynamic (MHD) simulations. The anisotropy in the turbulent fluctuations is mediated primarily by the mean, ambient or local magnetic field. The latter leads to a disparity in the spectral transfer of energy along and across the mean magnetic field. While the anisotropic cascades give rise to the relationship \tilde{λ}_∥ ∝ \tilde{λ}_\perp^{2/3} between the parallel (\tilde{λ}_∥ ~ 1/k_∥) and perpendicular (\tilde{λ}_\perp ~ 1/k_\perp) length-scales of the eddies relative to the mean 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 turn over time scales 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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