The Transition to Incompressibility from Compressible Magnetohydroynamic Turbulence

Details The Transition to Incompressibility from Compressible Magnetohydroynamic Turbulence The Transition to Incompressibility from Compressible Magnetohydroynamic Turbulence

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...640l.195s&link_type=abstract

The Astrophysical Journal, Volume 640, Issue 2, pp. L195-L198.

Astronomy and Astrophysics

Astronomy

17

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

Scientific paper

On the basis of three-dimensional time-dependent numerical simulations, we find that compressible magnetohydrodynamic fluids describing super-Alfvénic, supersonic, and strongly magnetized space and laboratory plasmas decay progressively to a state of near-incompressibility, characterized by a subsonic turbulent Mach number. This transition is mediated dynamically by disparate spectral energy dissipation rates in compressible magnetosonic and shear Alfvénic modes. Dissipation leads to super-Alfvénic turbulent motions decaying to a sub-Alfvénic regime that couples weakly with (magneto-) acoustic cascades. Consequently, the supersonic plasma motion dissipates into highly subsonic motion and density fluctuations experience a passive convection.

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