The perpendicular diffusion coefficient in collisionless astrophysical plasmas follows from three heuristic rules, yielding a new collisionless Rechester-Rosenbluth limit and identifying the parameter a^2 as the squared ratio of the ultra-scale to the bendover scale.
If, on the other hand, t‖ < t FL < t F luid the field lines become diffusive before condition (3) is met
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Heuristic Description of Perpendicular Diffusion of Energetic Particles in Astrophysical Plasmas
The perpendicular diffusion coefficient in collisionless astrophysical plasmas follows from three heuristic rules, yielding a new collisionless Rechester-Rosenbluth limit and identifying the parameter a^2 as the squared ratio of the ultra-scale to the bendover scale.