View of the neutral magnesium cloud from above of the orbital plane in the best-fit simulation (C-scenario). Because of the high density below the exobase (R_exo = 2 R_p; dashed orange circle) magnesium atoms escape more easily from the limbs of the atmosphere, unshielded from radiation pressure (the star is toward the top of the plot). The orange lines show the average trajectory of these flows. Gravitational effects and the lower velocity of the planetary wind prevent the cometary tail from dispersing as in the G-scenario (Fig. 13). The red line shows the average trajectory of the flow of particles emanating from shielded regions. Deviated by planetary gravity, the flow emerges from the cloud to the rear of the planet, where it becomes subjected to radiation pressure.