The evolution of gaseous planets is a complex process influenced by various physical parameters and processes. In this study, we present critical modifications to the Modules for Experiments in Stellar Astrophysics ( code to enhance its applicability to giant planet modeling. We introduce an equation of state (EoS) specifically tailored for materials at planetary conditions. The equation of state considers the thermodynamic properties of hydrogen-helium mixtures and heavy elements, improving the accuracy of internal structure calculations. We also present modifications to the radiative opacity to allow the modeling of grains, clouds and opacity windows. Furthermore, we refine the treatment of convective mixing processes in to better replicate convective mixing with the presence of composition gradients. Finally, we add a treatment for helium rain and settling. These modifications aim to enhance the predictive capabilities of for giant planet evolution and are publicly available. We hope that these improvements will lead to a deeper understanding of giant planet evolution in the Solar System and beyond.
Helled et al. (2025) studied this question.