Protoplanetary disks around magnetised young stars with large-scale magnetic fields - I. Steady-state solutions

Open Access

Fig. B.1.

Profiles of the vertically conductivity-averaged resistivity, $\bar{\bar{η}}$ ${\bar{{\bar{\eta}}}}$ , if calculated with a varying number of vertical layers. The three layers at z = 0, z = H_p, and z = z_B are always included, whereas the number of intermediate layers between z = H_p and z = z_B is varied. The layers are distributed evenly in the vertical direction between H_p and z_B.

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