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Detailed Reference Information |
Bhattacharjee, A., Ng, C.S., Ghosh, S. and Goldstein, M.L. (1999). A comparative study of four-field and fully compressible magnetohydrodynamic turbulence in the solar wind. Journal of Geophysical Research 104: doi: 10.1029/1999JA900327. issn: 0148-0227. |
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A four-field system of equations has been recently derived from the compressible magnetohydrodynamic (MHD) equations to describe turbulence in the solar wind. These equations apply to a plasma permeated by a spatially varying mean magnetic field when the plasma beta is of the order unity or less. In the presence of spatial inhomogeneities, the four-field equations predict pressure fluctuations of the order of the Mach number of the turbulence, as observed by Helios 1 and 2. It is shown that inhomogeneities that occur only in the form of pressure-balanced structures cannot account for density fluctuations as large as the Mach number of the turbulence. Numerical predictions from the four-field and compressible MHD equations are compared using the same initial condition. The comparison shows that the predictions of the four-field model are qualitatively consistent with the predictions of the compressible MHD model and suggests that the four-field model is a viable model of compressible turbulence in the solar wind. ¿ 1999 American Geophysical Union |
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Abstract |
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Keywords
Interplanetary Physics, MHD waves and turbulence, Interplanetary Physics, Plasma waves and turbulence, Interplanetary Physics, Solar wind plasma, Magnetospheric Physics, Polar cap phenomena, Space Plasma Physics, Waves and instabilities |
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Publisher
American Geophysical Union 2000 Florida Avenue N.W. Washington, D.C. 20009-1277 USA 1-202-462-6900 1-202-328-0566 service@agu.org |
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