Speaker
Description
Transverse transport of cosmic rays in a turbulent environment can be greatly influenced by the behavior of magnetic field lines. Indeed, in the limit of infinitely small Larmor radius, charged particles would exactly follow magnetic field lines. In particular the behavior of the spread of a bundle of field lines can have consequences in several astrophysical environments. In this talk we revisit the transverse diffusion of magnetic field lines, on two folds : (i) Numerically : we perform 3 dimensional synthetic turbulence simulations is various conditions and reconstruct the running field line diffusion coefficient of the separation between two field lines , (ii) Analytically : we try to reproduce the statistics of field line separation by applying a non-perturbative method and using the Corrsin’s independence hypothesis.
The links of these results with realistic MHD simulations will be also highlighted.