Interior models of Jupiter, Saturn and Neptune

Interior model calculations of Jupiter, Saturn and Neptune require EOS-data of hydrogen, helium and water in the regime of warm dense matter. In case of Saturn, the pressure in the deep interior rises up to 15 Mbar at 600010000 K and a hydrogen mass fraction of at least 40%. In Jupiter, due to his larger total mass compared to Saturn, the high-pressure region is more extended with pressures up to 40 Mbar at 15000-22000 K and a hydrogen mass fraction of at least 60%. In Neptune, icy condensates from the protosolar cloud provide the main component with pressures up to 8 Mbar at 5000-6000 K. Precise values depend on error bars of observational contstraints and on the equation of state (EOS) used for modeling. The lack of consistency of models of Jupiter with these constraints has been a longstanding problem which imposes strong conditions on the H-EOS [1, 2]; the only successfully applied so far is that of [3].