Balanced and Imbalanced MHD Turbulence: Models vs Numerics

Details Balanced and Imbalanced MHD Turbulence: Models vs Numerics Balanced and Imbalanced MHD Turbulence: Models vs Numerics

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21630906b&link_type=abstract

American Astronomical Society, AAS Meeting #216, #309.06; Bulletin of the American Astronomical Society, Vol. 41, p.872

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We review current state regarding models of MHD turbulence and present recent numerical results testing these models. We demonstrate that some models are grossly inconsistent with numerics. A correct model depicting MHD turbulent cascade, especially imbalanced cascade, is essential for understanding most astrophysical phenomena, such as star formation in turbulent galactic disk, properties of stellar winds and AGN jets. Such properties of MHD cascade as spectrum and anisotropy are essential for understanding both large-scale and small scale phenomena, heating, cosmic ray scattering and acceleration and many others. We have robust numerical bounds of these important properties, in particular we have a dependence of the total dissipation rate vs degree of imbalance.

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