Castillo-Rogez, Julie C.Julie C.Castillo-RogezHesse, M. A.M. A.HesseFORMISANO, MichelangeloMichelangeloFORMISANOSizemore, H.H.SizemoreBland, M.M.BlandErmakov, A. I.A. I.ErmakovFu, R. R.R. R.Fu2021-02-252021-02-2520190094-8276http://hdl.handle.net/20.500.12386/30609We propose a new internal evolution model for the dwarf planet Ceres matching the constraints on Ceres' present internal state from the Dawn mission observations. We assume an interior differentiated into a volatile-dominated crust and rocky mantle, and with remnant brines in the mantle, all consistent with inferences from the Dawn geophysical observations. Simulations indicate Ceres should preserve a warm crust until present if the crust is rich in clathrate hydrates. The temperature computed at the base of the crust exceeds 220 K for a broad range of conditions, allowing for the preservation of a small amount of brines at the base of the crust. However, a temperature ≥250 K, for which at least 1 wt.% sodium carbonate gets in solution requires a crustal abundance of clathrate hydrates greater than 55 vol.%, a situation possible for a narrow set of evolutionary scenarios.STAMPAenArticle10.1029/2018GL0814732-s2.0-85061262335000461855600009https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2018GL0814732019GeoRL..46.1963CFIS/05 - ASTRONOMIA E ASTROFISICA