Same as Figure 18 but for the three known planets (with best-fit masses) and a hypothetical fourth planet in between L 98-59 c and L 98-59 d, with a mass of 2.5 M⊕ and a period of 5.7 days. All four planets are on initially circular orbits (upper panel) or on initially eccentric orbits with e = 0.1 (lower panels). While the system is dynamically stable for the duration of the integrations in the former case, it quickly becomes unstable in the latter.