Other
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh11a0251d&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #SH11A-0251
Other
7509 Corona, 7827 Kinetic And Mhd Theory, 7863 Turbulence (4490)
Scientific paper
Comparisons of low Mach number compressible three-dimensional magnetohydrodynamic (CMHD3D) turbulence in the presence of a strong mean magnetic field and reduced magnetohydrodynamics (RMHD) are performed using pseudospectral numerical simulations. Different initial conditions are chosen to study how close the RMHD solution remains to the full compressible MHD solution as both freely evolve in time. When the initial state is prepared to satisfy the conditions assumed in the derivation of RMHD, namely, a strong mean magnetic field, and plane-polarized fluctuations, varying weakly along the mean magnetic field, simulations show that RMHD and CMHD3D evolve almost indistinguishably from one another. When some of the conditions are relaxed the agreement worsens but RMHD remains fairly close to CMHD3D, especially when the mean magnetic field is large enough. Mean energy, square current, vorticity and energy spectrum from the two solutions are compared and point-to-point separation estimations are computed. The results give support to the use of RMHD as an approximation of compressible MHD with a mean magnetic field under certain but quite practical conditions, like those found in the solar corona and wind.
Dmitruk Pablo
Matthaeus William H.
Oughton Sean
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