Furthermore, recent theoretical (C. Dorn & T. Lichtenberg 2021; N. Madhusudhan et al. 2021; H. Innes et al. 2023)and observational findings (R. Luque & E. Palle 2022;N. Madhusudhan et al. 2023; B. Benneke et al. 2024a;M. Holmberg & N. Madhusudhan 2024) support greater compositional diversity within the sub-Neptune population. While the coolest planets may be “Hycean worlds” with water in condensed liquid/ice phases under a H/He atmosphere, the warmer temperature of the vast majority of planets would instead imply a supercritical state for the water/volatile layer. Contrary to liquid water, supercritical water is highly miscible with hydrogen. Such warm, volatile-rich planets may therefore host exposed “mixed” envelopes where both H2 and potentially large amounts of HMMW volatiles coexist (B. Benneke et al.2024a; R. Burn et al. 2024; N. F. Wogan et al. 2024). In addition, water is expected to partition between the planetary envelope, the molten or solid mantle, and the metal core, leading to more uncertainties in planetary structure models(C. Dorn & T. Lichtenberg 2021; H. E. Schlichting &E. D. Young 2022; H. Luo et al. 2024).