Thermochemical modeling of gas and ice giant planets

Understanding the processes that lead to the formation of giant planets in planetary systems is crucial, because these planets are the architects of more complex systems harbouring rocky planets that form over longer timescales. Measuring the deep elemental abundances of giant planets is one of the keys to constrain their formation. After the Galileo probe measurements at Jupiter, Juno is making observations to constrain the deep oxygen abundance of the planet. Fewer measurements are available at Saturn, and even more so at Uranus and Neptune. The lack of in situ probes or sensitive enough remote sensing measurements planned for these planets, thermochemical computations offers the means to help constrain the deep elemental abundances by reproducing the abundances of observable minor species which are chemically linked with the deep and main reservoirs of the main elements. This is particularly true for oxygen, which is mainly carried by water, a condensible species in giant planet atmospheres. Water ice trapped the other heavy elements during planetesimal formation beyond the snowline. The ratios between oxygen and the other elements bear implications on the form under which water condensed beyond the snowline (amorphous ice vs. clathrates). 
In this paper, we will present and discuss the results of our model for the solar system giant planets and compare the situations of gas vs. ice giant planets.