DOE OSTI2016
In astrophysical plasmas, the magnetic field line random walk (FLRW) plays an important role in guiding particle transport. The FLRW behavior is scaled by the Kubo number R=(b/B{sub 0})(ℓ{sub ∥}/ℓ{sub ⊥}) for rms magnetic fluctuation b, large-scale mean field B{sub 0}, and coherence scales parallel (ℓ{sub ∥}) and perpendicular (ℓ{sub ⊥}) to B{sub 0}. Here we use a nonperturbative analytic framework based on Corrsin’s hypothesis, together with direct computer simulations, to examine the R-scaling of the FLRW for varying B {sub 0} with finite b and isotropic fluctuations with ℓ{sub ∥}/ℓ{sub ⊥}=1, instead of the well-studied route of varying ℓ{sub ∥}/ℓ{sub ⊥} for b ≪B{sub 0}. The FLRW for isotropic magnetic fluctuations is also of astrophysical interest regarding transport processes in the interstellar medium. With a mean field, fluctuations may have variance anisotropy, so we consider limiting cases of isotropic variance and transverse variance (with b {sub z} = 0). We obtain analytic theories, and closed-form solutions for extreme cases. Padé approximants are provided to interpolate all versions of theory and simulations to any B {sub 0}. We demonstrate that, for isotropic turbulence, Corrsin-based theories generally work well, and with increasing R there is a transition from quasilinear to Bohm diffusion. This holds even with b {sub z} = 0, when different routes to R→∞ are mathematically equivalent; in contrast with previous studies, we find that a Corrsin-based theory with random ballistic decorrelation works well even up to R = 400, where the effects of trapping are barely perceptible in simulation results.
79 ASTRONOMY AND ASTROPHYSICS↗