Factors Affecting the Rheologic Properties of Martian Polar Ice

Mathematics – Logic

Scientific paper

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Ice, Mars (Planet), Mars Surface, Polar Caps, Rheology, Temperature, Hydrates, Water, Gravitational Fields, Dust, Carbon Dioxide

Scientific paper

The flow of the martian polar ice caps is influenced by the martian gravity field, the physical configuration of the caps and the underlying hard terrain, and the distribution and rheology of the material in the caps. This contribution speaks to the intrinsic theology of the material that comprises the polar caps. The polar caps are a mixture of phases of H2O, CO2, and rock. There is great uncertainty in the relative proportions of these components, and there are probably differences between compositions of the north and south polar caps. Frozen CO2 may exist as a shallow surface frost, especially on the south polar cap, but probably does not persist in rheologically important quantities. A good case can be made that CO2 is present as clathrate hydrate, and indeed, much of the material below a meter or so in the ice caps lies within the stability field Of CO2 hydrate. The amount of hydrate is difficult to predict, and the ratio of dust to ice in the layered deposits is not known to within several orders of magnitude. Finally, not only is the proportion of phases in the ice caps largely unknown, it is also likely to be nonuniform, as shown by layered deposits visible in sectional exposures at both poles. We assume for the purposes of discussion the simplest picture of the martian ice caps as void-free, predominantly water ice 1, with some clathuate hydrates and dust mixed in. The rheology of water ice is fairly well known, the rheology of hydrates is poorly known, and the dust can be safely assumed to be nondeformable in this mixture. To the extent the simple picture is incorrect (for example, if hydrates are present in very large quantities), the exercise here become less useful.

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