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High-resolution subsurface water-ice distributions on Mars

Abstract

Theoretical models indicate that water ice is stable in the shallow subsurface (depths of <1–2 m) of Mars at high latitudes1,2,3,4,5,6,7. These models have been mainly supported by the observed presence of large concentrations of hydrogen detected by the Gamma Ray Spectrometer suite of instruments on the Mars Odyssey spacecraft8,9,10. The models and measurements are consistent with a water-ice table that steadily increases in depth with decreasing latitude. More detailed modelling has predicted that the depth at which water ice is stable can be highly variable, owing to local surface heterogeneities such as rocks and slopes, and the thermal inertia of the ground cover11,12,13. Measurements have, however, been limited to the footprint (several hundred kilometres) of the Gamma Ray Spectrometer suite, preventing the observations from documenting more detailed water-ice distributions. Here I show that by observing the seasonal temperature response of the martian surface with the Thermal Emission Imaging System on the Mars Odyssey spacecraft14, it is possible to observe such heterogeneities at subkilometre scale. These observations show significant regional and local water-ice depth variability, and, in some cases, support distributions in the subsurface predicted by atmospheric exchange and vapour diffusion models. The presence of water ice where it follows the depth of stability under current climatic conditions implies an active martian water cycle that responds to orbit-driven climate cycles15,16,17. Several regions also have apparent deviations from the theoretical stability level, indicating that additional factors influence the ice-table depth. The high-resolution measurements show that the depth to the water-ice table is highly variable within the potential Phoenix spacecraft landing ellipses, and is likely to be variable at scales that may be sampled by the spacecraft.

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Figure 1: Modelled temperatures for a variety of surface cover thermal inertias (top layer inertia) and ice-table depths, at 67.5°N.
Figure 2: Ice depth map centred near 67.5° N, 132° E (Phoenix B region proposed landing site).
Figure 3: Modelled temperatures at 05:00 for the surfaces shown in Fig. 2 .
Figure 4: Ice depth map centred near 67° S, 36.5° E.

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Acknowledgements

Thanks to P. Christensen, R. Fergason, H. Kieffer, C. Edwards, R. Luk, K. Bender, and J. Hill for data processing and targeting help and discussions.

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Correspondence to Joshua L. Bandfield.

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Bandfield, J. High-resolution subsurface water-ice distributions on Mars. Nature 447, 64–67 (2007). https://doi.org/10.1038/nature05781

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