Theory and Transport of Nearly Incompressible Magnetohydrodynamic Turbulence

• Published in: The Astrophysical journal Vol. 835; no. 2; pp. 147 - 176
• Main Authors: Zank, G. P., Adhikari, L., Hunana, P., Shiota, D., Bruno, R., Telloni, D.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.02.2017; IOP Publishing
• Subjects: Astrophysics; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COMPARATIVE EVALUATIONS; Computational fluid dynamics; COMPUTERIZED SIMULATION; COUPLINGS; DENSITY; EQUATIONS; FLUCTUATIONS; Fluid flow; FORECASTING; Incompressibility; Interstellar matter; Interstellar medium; Magnetohydrodynamic turbulence; MAGNETOHYDRODYNAMICS; magnetohydrodynamics (MHD); NONLINEAR PROBLEMS; PLASMA; SOLAR WIND; Solar wind turbulence; SPECTRA; Transport; TURBULENCE; waves
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/835/2/147

The theory of nearly incompressible magnetohydrodynamics (NI MHD) was developed largely in the early 1990s, together with an important extension to inhomogeneous flows in 2010. Much of the focus in the earlier work was to understand the apparent incompressibility of the solar wind and other plasma environments, and the relationship of density fluctuations to apparently incompressible manifestations of turbulence in the solar wind and interstellar medium. Further important predictions about the "dimensionality" of solar wind turbulence and its relationship to the plasma beta were made and subsequently confirmed observationally. However, despite the initial success of NI MHD in describing fluctuations in the solar wind, a detailed application to solar wind turbulence has not been undertaken. Here, we use the equations of NI MHD to describe solar wind turbulence, rewriting the NI MHD system in terms of Elsässer variables. Distinct descriptions of 2D and slab turbulence emerge naturally from the Elsässer formulation, as do the nonlinear couplings between 2D and slab components. For plasma beta order 1 or less regions, predictions for 2D and slab spectra result from the NI MHD description, and predictions for the spectral characteristics of density fluctuations can be made. We conclude by presenting a NI MHD formulation describing the transport of majority 2D and minority slab turbulence throughout the solar wind. A preliminary comparison of theory and observations is presented.