An inventory of major volatiles trapped in Ceres

Details An inventory of major volatiles trapped in Ceres An inventory of major volatiles trapped in Ceres

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sf2a.conf...85m&link_type=abstract

SF2A-2004: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 14-18, 2004. Edited by F. Combes, D. Barret

Astronomy and Astrophysics

Astrophysics

Scientific paper

We determine the nature and the composition of ices incorporated in the interior of Ceres, assuming that icy planetesimals produced beyond 5 AU in the solar nebula took part in its formation (Cyr et al. 1998). We argue that volatiles were trapped under the forms of clathrate hydrates and hydrates in the outer solar nebula prior to have been incorporated in icy planetesimals and subsequently in Ceres. Under the assumption that planetesimals that formed Ceres did not outgas during its accretion phase and its thermal evolution, we predict the per mass abundances with respect to H2O of CO, CH4, N2, NH3, Ar, Kr, and Xe in the interior of the asteroid. The prediction of the presence of ammonia in Ceres is compatible with the hypothesis of existence of a deep liquid layer (McCord and Sotin 2004) and may be tested by the DAWN space mission in 2014.

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