NEARLY INCOMPRESSIBLE FLUIDS .2. MAGNETOHYDRODYNAMICS, TURBULENCE, AND WAVES

The theory of nearly incompressible (NI) fluid dynamics developed previously for hydrodynamics is extended to magnetohydrodynamics (MHD) On the basis of a singular expansion technique, modified systems of fluid equations are derived for which the effects of compressibility are admitted only weakly in terms of the different possible incompressible solutions (thus ''nearly incompressible MHD''). NI MHD represents the interface between the compressible and incompressible magnetofluid descriptions in the subsonic regime. The theory developed here does not hold in the presence of very large thermal, gravitational, or field gradients. It is found that there exist three distinct NI descriptions corresponding to each of the three possible plasma beta (beta = the ratio of thermal to magnetic pressure) regimes (beta much less than 1, beta approximately 1, beta much greater than 1). In the beta much greater than 1 regime, the compressible MHD description converges in the low Mach number limit to the equations of classical incompressible three-dimensional (3-D) MHD. However, for the remaining plasma beta regimes, the imposition of a large dc magnetic field forces the equations of fully compressible 3-D MHD to converge to the equations of 2-D incompressible MHD in the low Mach number limit. The ''collapse in dimensionality'' corresponding to the different plasma beta regimes clarifies the distinction between the 3-D and 2-D incompressible MHD descriptions (and also that of 2 1/2-D incompressible MHD). The collapse in dimensionality that occurs as a result of a decreased plasma beta can carry over to the weakly compressible corrections. For a beta approximately 1 plasma, Alfven waves propagate parallel to the applied magnetic field (reminiscent of reduced MHD), while for a beta much less than 1 magnetofluid, quasi-1-D long-wavelength acoustic modes propagate parallel to the applied magnetic field. The detailed theory of weakly compressible corrections to the various incompressible MHD descriptions is presented and the implications for the solar wind emphasized.