Ratio of density between gas in the wind (spherical outward motion) to that in the belt (in Keplerian motion in the belt), at the belt location, R, as a function of the stellar wind mass-loss rate. For this plot, we use Eq. (10) with µ = 28, υ_sw = 100 km/s, R = 100 au, ΔR = 50 au, σ_col = 2 × 10⁻¹⁸ m², and H = 0.05R. For a stellar wind mass-loss rate that is a few tens of that of the Sun, values of n_w become greater than n_d and the wind becomes dominant.