Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.1314m&link_type=abstract
American Astronomical Society, DPS meeting #38, #13.14; Bulletin of the American Astronomical Society, Vol. 38, p.507
Astronomy and Astrophysics
Astronomy
1
Scientific paper
The trapping of volatile species in the form of clathrate hydrates during the formation of icy planetesimals in the outer solar nebula is a realistic mechanism to interpret the volatile enrichments observed in the giant planets. However, up until now, some ad hoc assumptions have been made in the scenarios using clathration as the main process to allow the trapping of volatiles in the solar nebula gas-phase. In particular, the clathration process is always assumed to be fully efficient. Moreover, the abundance of oxygen is still considered as a free parameter adjusted in order to provide enough water to trap as clathrate hydrate the required volatile species in the outer nebula. In this work, we address these shortcomings and we demonstrate that it is possible to fit the volatile enrichments in Jupiter and Saturn by postulating a partial efficiency of the clathration process and using an oxygen solar abundance. We also show that the volatile species that are not trapped via clathration crystallize as pure condensates at the temperature and pressure conditions of the outer solar nebula. Icy planetesimals formed in the outer nebula then incorporate volatiles trapped both in the form of clathrate hydrates and pure condensates. We finally show that the resulting quantities of volatiles contained within the envelopes of Jupiter and Saturn are compatible with the amounts of heavy elements (ices + rocks) predicted by their internal structure models.
Marboeuf Ulysse
Mousis Olivier
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