Further simulation results for the disc gap at 75 au and δ = 10⁻⁴. (a) e-m time sequence, showing that a small number of massive cores are formed, which excite and prevent the growth of the latecomers. This is similar to the results to the case with r₀ = 10 au and δ = 10⁻⁴. (b) i-m plot at the end of the simulations, showing that the inclinations remain very low for all bodies, i.e. around the values drawn at their formation, (c) Differential mass distribution at the end also shows only a small number of massive cores are formed and the simulations are stopped before a large population of planetesimals is produced. This is also similar to the case with r₀ = 10 au and δ = 10⁻⁴.