Comparison of the radius and interior–atmosphere boundary temperature between our fc-correlated model (MSEIRADTRAN) and that of Pluriel et al. (2019). Left panel: mass-radius relationships for a planet with a water-dominated atmosphere orbiting a Sun-like star at a_d = 0.05 AU. Dashed lines indicate the total radius calculated by MSEIRADTRAN, while the solid line corresponds to the interior radius, which comprises the core, mantle, and supercritical water (SW) hydrosphere. Triangles and circles indicate the total radius and the interior radius obtained when the interior model is coupled with the atmospheric model of Pluriel et al. (2019), respectively. Right panel: temperature at the 300 bar interface as a function of planetary mass.