Table 5
Overview of the time and size intervals for the aqueous alteration, water-dust differentiation and water retention in icy planetesimalsas well as for the water content and the structures of the bodies Ceres accreted from, for different formation scenarios.
| Outcome | Asteroid belt | Inter-planet disk | Kuiper belt (3 : 1) | Kuiper belt (1 : 1) |
|---|---|---|---|---|
| Alteration | tac ≥ 1−1.9 Myr | tac ≥ 1−1.8 Myr | R > 70 km | R > 110 km |
| R < 10−200 km | R < 10−200 km | |||
| Differentiation | tac ≤ 1.6−5 Myr | tac ≤ 1.5−5 Myr | R ≥ 175−190 km | No |
| R ≥ 10−150 km | R ≥ 10−170 km | |||
| Water retention | tac ≥ 1−1.9 Myr | tac ≥ 1−1.8 Myr | All | All |
| R < 10−200 km | R < 10−200 km | |||
| Ceres’ material | Dry + wet | Dry + wet | Wet only | Wet only |
| Structures | 1−6 | 1−6 | 1−4 | 1, 2 |
Notes. The structures correspond to those numbered in Fig. 4. The term “wet” stands for both altered and unaltered bodies that contain an H2 O fraction. The term “dry” stands for bodies that have lost their H2O fraction.
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