Using ab initio molecular dynamics simulations, we recently calculated equations of state for the main constituents of planetary interiors: H, He, H2O, MgSiO3(MgO,SiO2) and Fe. These equations of states are multi-phases, include liquid and solid phases, and aim at building benchmark planetary and exoplanetary interior models solely based on ab initio predictions. This talk will concentrate on Jupiter. We will review how our current understanding of the behavior of these basic constituents at extreme density temperature conditions modifies our current understanding of Jupiter interior, not only for the envelop where metallization of hydrogen and hydrogen-helium demixing is the issue but also for the core where the high-pressure melting properties of iron, water, and silicates bring a new understanding on the nature of giant planet cores.
This work is supported by the University Paris Sciences et Lettres (PSL) and the IRIS project Origines and conditions for the emergence of life, and the the French Agence National de la Recherche under contract PLANETLAB ANR-12-BS04-0015.