Modelling the internal structure of Ceres: Coupling of accretion with compaction by creep and implications for the water-rock differentiation

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Table 4

Data describing the circumstances of compaction at the centre of the proto-Ceres for t₀ = 1 Ma relative to CAIs and t_ac = 2 Ma.

Model	Mineral	Time	Temperature	Radius	Porosity	Dehydration

CIa	Serpentine	1.007−1.024	200−270	1.265−1.294	48−30	775
high-	Montmorillonite	1.033−1.040	300−322	1.304−1.315	30−18	1070
density	Epsomite	1.320−1.530	587−720	2.875−5.410	8−0	353
model	Mirabilite	1.050−1.062	350−375	1.334−1.367	18−13	305
from (1)	Pyrene	1.007−1.024	200−270	1.265−1.294	48−30	−
and (2)	Halite	1.033−1.040	300−322	1.304−1.315	30−18	−
	Magnetite	1.120−1.220	445−526	1.569−2.117	13−8	−

CIb	Saponite	1.007-1.038	200−317	1.265−1.359	48−33	1073
low-	Epsomite	1.216−1.284	710−782	2.241−2.750	20−0	353
density	Mirabilite	1.042−1.057	330−377	1.364−1.409	33−28	305
model	Pyrene	1.007−1.038	200−317	1.265−1.359	48−33	−
from (1)	Gypsum	1.172−1.190	550−670	1.712−2.068	28−25	423
and (2)	Hematite	1.190−1.216	670−710	2.070−2.241	25−20	−

Notes. All times are given relative to the formation of CAIs (and include the accretion onset time t₀ = 1 Ma). See Sect. 3.1 and Fig. 3 for further information.

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