Will Ceres turn out to be a rocky asteroid or rocky dwarf planet?
Will it be porus or perhaps geode like?
Ceres’s oblateness is inconsistent with an undifferentiated body, which indicates that it consists of a rocky core overlain with an icy mantle. This 100-kilometer-thick mantle (23%–28% of Ceres by mass; 50% by volume) contains 200 million cubic kilometers of water, which is more than the amount of fresh water on Earth. This result is supported by the observations made by the Keck telescope in 2002 and by evolutionary modeling. Also, some characteristics of its surface and history (such as its distance from the Sun, which weakened solar radiation enough to allow some fairly low-freezing-point components to be incorporated during its formation), point to the presence of volatile materials in the interior of Ceres.
Alternatively, the shape and dimensions of Ceres may be explained by an interior that is porous and either partially differentiated or completely undifferentiated. The presence of a layer of rock on top of ice would be gravitationally unstable. If any of the rock deposits sank into a layer of differentiated ice, salt deposits would be formed. Such deposits have not been detected. Thus it is possible that Ceres does not contain a large ice shell, but was instead formed from low-density asteroids with an aqueous component. The decay of radioactive isotopes may not have produced sufficient heat to cause differentiation.
Ceres Physical characteristics Internal structure
Ceres has a density of 2.09 grams per cubic centimeter, leading scientists to conclude approximately a quarter of its weight is water. This would give the dwarf planet more fresh water than Earth contains.
The thin, dusty crust is thought to be composed of rock, while a rocky inner core lies at the center.
Ceres: The Smallest and Closest Dwarf Planet
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