We calculate electronic opacities along the pressure-temperature conditions of Jupiter's and Saturn's interior by using ab initio molecular dynamics simulations based on density functional theory. We evaluate the Kubo–Greenwood formula for the dynamic conductivity, derive the absorption coefficient and the electronic thermal conductivity, and, thereby, the electronic opacity via the dielectric function. The opacity determines the effectiveness of heat transport mechanisms from the hot center to the cool surface of a planet. Our results will inform interior and thermal evolution models for Jupiter and Saturn as prototypical gas giant planets, in particular for the region of warm dense matter in their deep interior, where quantum and correlation effects are important.
Preising et al. (Fri,) studied this question.