Line-forming radii for the hot Jupiter planet around a G2 star for different outflow profiles and with calculations truncated at 4 R_p. The top panel shows the density and velocity profiles (dashed). The second panel shows the result for a Parker wind profile with Ṁ = 10¹⁰ g s⁻¹ and T = 8000 (same system as in the upper right panel of Fig. 3, but now stopped below the Hill radius). The third panel shows the result for a Parker wind profile with Ṁ = 10¹¹ g s⁻¹ and T = 8000. The bottom panel shows the results for ATES, which predicted a mass-loss rate of Ṁ = 10¹¹ g s⁻¹. We find additional lines at small radii (≲1.1 R_p) when using ATES because its density profile increases steeply in the lower atmosphere.