Detection of local H 2 O exposed at the surface of Ceres
13. Climate action
0103 physical sciences
01 natural sciences
DOI:
10.1126/science.aaf3010
Publication Date:
2016-09-01T18:54:29Z
AUTHORS (12)
ABSTRACT
INTRODUCTION
Dwarf planet Ceres’ low average-density (2162 ± 3 kg m
−3
) indicates that it must contain considerable water. Water is likely a key component in the chemical evolution and internal activity of Ceres, possibly resulting in a layer of ice-rich material and perhaps liquid in the mantle. Mineral hydroxides (OH-bearing) and hydrates (H
2
O-bearing), such as clays, carbonates, and various salts, would be created. These hypotheses were supported by the detection of hydroxyl (OH)–rich materials, OH-bearing molecule releases, H
2
O vapor molecules, and haze. However, the presence of H
2
O on the surface has not previously been confirmed. The detection and mapping of H
2
O on Ceres is one objective of the Dawn spacecraft, in orbit around Ceres since March 2015.
RATIONALE
The purpose of the Dawn space mission at Ceres is to study the geology, geophysics, and composition remotely by means of high-resolution imagery and spectrometry. Dawn’s Visible and InfraRed Mapping Spectrometer (VIR) measures the sunlight scattered by the surface of Ceres in a range of wavelengths between 0.25 and 5.1 μm. The position and shape of absorption features in VIR reflectance spectra are sensitive to the surface mineral and molecular composition. In spectroscopy, absorption bands at 2.0, 1.65, and 1.28 μm are characteristic of vibration overtones in the H
2
O molecule.
RESULTS
Dawn has detected water-rich surface materials in a 10-km-diameter crater named Oxo, which exhibit all absorption bands that are diagnostic of the H
2
O molecule (see the figure). These spectra are most similar to those of H
2
O ice, but they could also be attributable to hydrated minerals. Oxo crater appears to be geologically very young (~1 million to 10 million years); it has sharp rims and its floor is almost devoid of impacts, suggesting a recent exposure of surface H
2
O. The high latitude and morphology of the Oxo crater protects much of the surface area from direct solar illumination for most of the cerean day, presenting favorable conditions for the stability of water ice or heavily hydrated salts.
CONCLUSION
Four ways to create or transport H
2
O on Ceres are considered: (i) Exposure of near-surface H
2
O-rich materials by a recent impact or an active landslide seems most consistent with the presence of both mineral hydrates and water ice. (ii) Release of subsurface H
2
O may occur on Ceres, similar to release on comet nuclei, but may never recondense on the surface. (iii) Infall of ice-bearing objects is not likely to deposit water on Ceres, because the H
2
O molecule likely would dissociate upon impact. (iv) Implantation of protons from the solar wind on the surface is not a probable origin of OH on Ceres because of the low flux of solar wind charged particles. We therefore conclude that surface H
2
O or hydrated minerals are the most plausible explanation.
Dawn VIR infrared observations of Oxo crater on Ceres demonstrate the detection of H
2
O at the surface.
(
A
) Reflectance spectrum collected where absorption bands of H
2
O at 1.28, 1.65, and 2 μm are the strongest (in blue) compared with a laboratory spectrum of H
2
O ice (black). The lab spectrum is scaled and vertically shifted for clarity. (
B
) Perspective view of Oxo crater observed by the Dawn Framing Camera (FC), where the two high-albedo areas right next to the scarps contain H
2
O-rich materials.
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