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Simulating Cosmic-Ray Diffusion Coefficients in the Presence of Synthetic Magnetic Turbulence with a Scalable Compressive Component: First Results for Heliosheath Parameters

  • Authors: J. S. Troskie, N. E. Engelbrecht

J. S. Troskie and N. E. Engelbrecht 2026 The Astrophysical Journal Supplement Series 286 .

  • Provider: AAS Journals

Caption: Figure 12.

Left panel: sample trajectories computed over the duration of one simulation for 70 MeV protons in a magnetic field for which (δB/B0) = 0.48, with B0 = 0.1 nT. The red line corresponds to a purely transverse turbulent component, while ﹩{(\delta {B}_{z}/\delta B)}^{2}=95 \% ﹩ for the blue line. Right panel: a small portion of the trajectory of a 70 MeV proton in the presence of a field statistically identical to that assumed in the left panel, but with all variance allocated to the compressive component. The total parallel displacement of the proton in the presence of the latter field extends to several thousand astronomical units (see Figure 6).

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