Magnetohydrodynamic turbulence and the associated spatial diffusion tensor of cosmic rays in dynamical galactic halos

Open Access

Fig. C.1

Contours of U_z and poloidal velocity vectors for the HI-base run when using a grid size equal to that of HI-80, with colored blocks indicating actual computational cells. Top: with zero-gradient boundary conditions at all outer boundaries. Bottom: additionally enforcing a no-inflow condition at z = z_max. The length of velocity arrows is directly proportional to $\sqrt{U_{R}^{2} + U_{z}^{2}}$ $\sqrt{U_{R}^{2}+U_{z}^{2}}$ in order to ease comparison with Fig. 3 of HI-80.

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