Time from formation until convergence to a core-envelope structure (rainout timescale) as a function of envelope mass, shown in green. Trend is shown for sub-Neptune planets that contain 6.7 M_⊕ of silicates and their gas (H,He) mass is determined by the mass loss rate, from 3.3 M_⊕ (original model, no mass loss) down to 0.33 M_⊕ (3 M_⊕ mass loss). In blue, we show the maximum radius inflation by rainout in comparison to the core-envelope structure model at the rainout timescale. Curves are polynomial fits for the evolution data points.