Abstract
Based on the microscopic formulation of transport processes, we derive a set of equations describing space-time evolution of the magnitudes and the spectral distributions of both the diagonal and off-diagonal elements of the magnetic-field fluctuation tensor for the plasmas in a disk geometry. Turbulence is generated mainly by the differential rotation of the plasmas; it decays through current dissipation due to anomalous magnetic viscosity. In the stationary state, the strengths of turbulence are expressed in terms of the macroscopic physical parameters of the system, such as the disk thickness and the rate of differential rotation; the wavenumber spectrum is proportional to k/sup -4/. The results are applied to the Galaxy, providing an essential account of the observed magnetic energy density. (AIP)
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