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|Title:||DYNAMICAL FIELD LINE CONNECTIVITY IN MAGNETIC TURBULENCE|
W. H. Matthaeus
Bartol Research Institute
|Keywords:||Earth and Planetary Sciences|
|Citation:||Astrophysical Journal. Vol.806, No.2 (2015)|
|Abstract:||© 2015. The American Astronomical Society. All rights reserved. Point-to-point magnetic connectivity has a stochastic character whenever magnetic fluctuations cause a field line random walk, but this can also change due to dynamical activity. Comparing the instantaneous magnetic connectivity from the same point at two different times, we provide a nonperturbative analytic theory for the ensemble average perpendicular displacement of the magnetic field line, given the power spectrum of magnetic fluctuations. For simplicity, the theory is developed in the context of transverse turbulence, and is numerically evaluated for the noisy reduced MHD model. Our formalism accounts for the dynamical decorrelation of magnetic fluctuations due to wave propagation, local nonlinear distortion, random sweeping, and convection by a bulk wind flow relative to the observer. The diffusion coefficient DXof the time-differenced displacement becomes twice the usual field line diffusion coefficient Dxat large time displacement t or large distance z along the mean field (corresponding to a pair of uncorrelated random walks), though for a low Kubo number (in the quasilinear regime) it can oscillate at intermediate values of t and z. At high Kubo number the dynamical decorrelation decays mainly from the nonlinear term and DXtends monotonically toward 2Dxwith increasing t and z. The formalism and results presented here are relevant to a variety of astrophysical processes, such as electron transport and heating patterns in coronal loops and the solar transition region, changing magnetic connection to particle sources near the Sun or at a planetary bow shock, and thickening of coronal hole boundaries.|
|Appears in Collections:||Scopus 2011-2015|
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