Distribution in longitude of the number of the flow lines that cross the sphere at a distance of 3 R_TS from the host star for the case V = 2 km s⁻¹, B = 7 µG, including the magnetic field of the host star (model 6). In the upper panel, the solid (dotted) lines show the numbers of the crossing points above (below) the (B, V) plane. The middle panel shows the sum of both. The lower panel shows the result for the case in which the stellar magnetic field is neglected (model 5).