Observations and thermochemical modeling of gas and ice giant planets
- 1Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, Pessac 33615, France (thibault.cavalie@u-bordeaux.fr)
- 2LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, Meudon, France.
- 3Cornell University, Ithaca, NY, USA
- 4Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
- 5Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), UMR CNRS 7583, Université Paris-Est-Créteil, Université de Paris, Institut Pierre Simon Laplace, Créteil, France
The formation of giant planets can mainly be explained by two models: core accretion and gravitational collapse. Measurements of magnetic and gravity fields, as well as deep composition can help to constrain which scenario led to the formation of the Solar System Giant Planets. The deep composition also holds keys to understanding how primordial ices condensed and trapped the heavy elements, in the form of pure condensates, amorphous ices or clathrates. While the Galileo probe enabled measuring the abundances of noble gases and other heavy elements in Jupiter, the elemental composition of Saturn and the Ice Giants remains poorly constrained. Observations coupled with thermochemical modeling can help us to constrain the deep composition of giant planets and can also be used in synergy with mass spectrometry measurements of an in situ probe.
In this paper, we will present recent results of thermochemical modeling of the Ice Giants and compare them with results obtained for Jupiter.
How to cite: Cavalié, T., Lunine, J., Mousis, O., and Venot, O.: Observations and thermochemical modeling of gas and ice giant planets, Europlanet Science Congress 2022, Granada, Spain, 18–23 Sep 2022, EPSC2022-33, https://doi.org/10.5194/epsc2022-33, 2022.
