Physics
Scientific paper
Dec 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh51c0284g&link_type=abstract
American Geophysical Union, Fall Meeting 2004, abstract #SH51C-0284
Physics
7863 Turbulence, 2149 Mhd Waves And Turbulence, 2164 Solar Wind Plasma
Scientific paper
The solar wind and the interstellar medium is permeated by large-scale magnetic fields that render magnetohydrodynamic (MHD) turbulence anisotropic. In the weak-turbulence limit in which three-wave interactions dominate, analytical and high-resolution numerical results based on random scattering of shear-Alfvén waves propagating parallel to a large-scale magnetic field demonstrate rigorously an anisotropic energy spectrum that scales as k⊥-2, instead of the famous Iroshnikov-Kraichnan spectrum of k-3/2 for the isotropic case. Even in the absence of a background magnetic field, when the energy spectrum is globally isotropic, anisotropy is found to develop with respect to the local magnetic field. Collisionless turbulence is studied in electron magnetohydrodynamics (EMHD), where whistler waves mediate the anisotropic energy cascade. Comparisons are made with MHD turbulence, especially with respect to global and local anisotropy in both inertial and dissipation ranges. The anisotropy of the energy cascade necessarily implies anisotropy of turbulent heating. Scalings of collisional and collisionless energy spectrum and dissipation rate will be discussed.
Bhattacharjee Anirban
Germaschewski Kai
Ng Cindy
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