Interior Models of Uranus and Neptune

摘要: "Empirical" models (pressure versus density) of Uranus and Neptune interiors constrained by the gravitational coefficients J 2, 4, planetary radii masses, Voyager solid-body rotation periods are presented. The empirical pressure-density profiles then interpreted in terms physical equations state hydrogen, helium, ice (H2O), rock (SiO2) to test plausibility models. compositions found be similar with somewhat different distributions high-Z material. big difference between two planets is that requires a non-solar envelope, while best matched solar composition envelope. Our analysis suggests heavier elements both Uranus' Neptune's interior might increase gradually toward centers. Indeed it possible fit moments without sharp compositional transitions.