Physics – Condensed Matter – Statistical Mechanics
Scientific paper
Nov 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280.107m&link_type=abstract
In JPL Solar Wind Five p 107-130 (SEE N84-13067 03-92)
Physics
Condensed Matter
Statistical Mechanics
14
Dynamic Models, Magnetohydrodynamic Flow, Mathematical Models, Plasma Turbulence, Solar Wind, Space Plasmas, Decay, Equations Of Motion, Fokker-Planck Equation, Homogeneity, Navier-Stokes Equation, Vlasov Equations
Scientific paper
The present state of MHD turbulence theory as a possible solar wind research tool is surveyed. The theory is statistical, and does not make statements about individual events. The ensembles considered typically have individual realizations which differ qualitatively, unlike equilibrium statistical mechanics. Most of the theory deals with highly symmetric situations; most of these symmetries have yet to be tested in the solar wind. The applicability of MHD itself to solar wind parameters is highly questionable; yet it has no competitors, as a potentially comprehensive dynamical description. The purpose of solar wind research require sharper articulation. If they are to understand radial turbulent plasma flows from spheres, laboratory experiments and numerical solution of equations of motion may be cheap alternative to spacecraft. If "real life" information is demanded, multiple spacecraft with variable separation may be necessary to go further. The principal emphasis in the theory so far has been on spectral behavior for spatial covariances in wave number space. There is no respectable theory of these for highly anisotropic situations. A rather slow development of theory acts as a brake on justifiable measurement, at this point.
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