Viscous flow features on the surface of Mars: Observations from high‐resolution Mars Orbiter Camera (MOC) images

@article{Milliken2003ViscousFF,
  title={Viscous flow features on the surface of Mars: Observations from high‐resolution Mars Orbiter Camera (MOC) images},
  author={Ralph E. Milliken and John F. Mustard and David L. Goldsby},
  journal={Journal of Geophysical Research},
  year={2003},
  volume={108},
  pages={5057}
}
(10 5 –10 7 years) of the material. Our shear stress estimates of 10 � 1.5 –10 � 2.5 MPa yield strain rates on the order of 10 � 11 –10 � 16 s � 1 , which are within the superplastic flow regime of ice. Mean annual surface temperatures, age constraints, and strain estimates show that it is possible for a meters-thick ice-dust mixture to undergo viscous deformation under past or present surface conditions for ice grain sizes >10 mm. The meters-thick layer in which the viscous flow features… 

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References

SHOWING 1-10 OF 56 REFERENCES

Geomorphic Evidence for the Distribution of Ground Ice on Mars

TLDR
High-resolution Viking orbiter images show evidence for quasi-viscous relaxation of topography, which suggests that ice at low latitudes has been lost via sublimation and diffusion through the regolith, thereby causing a net poleward transport of ice over martian history.

Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice

TLDR
Observational evidence for a mid-latitude reservoir of near-surface water ice occupying the pore space of soils is reported and it is inferred that the reservoir was created during the last phase of high orbital obliquity less than 100,000 years ago, and is now being diminished.

"Softened" Impact Craters on Mars: Implications for Ground Ice and the Structure of the Martian Megaregolith

Abstract "Terrain softening" is a distinct style of landform degradation observed on Mars. The morphology and distribution of softened terrain have led to the hypothesis that it is the result of

Recent ice ages on Mars

TLDR
Evidence is shown that dusty, water-ice-rich mantling deposits on Mars formed during a geologically recent ice age that occurred from about 2.1 to 0.4 Myr ago, a key pacemaker of ice ages on the Earth.

Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission

More than 3 years of high-resolution (1.5–20 m/pixel) photographic observations of the surface of Mars have dramatically changed our view of that planet. Among the most important observations and

Formation of Recent Martian Debris Flows by Melting of Near-Surface Ground Ice at High Obliquity

TLDR
It is shown that these gullies on Mars may result from the melting of water ice in the top few meters of the martian subsurface at high obliquity, and that above-freezing temperatures can occur in the near surface of Mars, but are only predicted at latitudes and for slope orientations corresponding to where the gullies have been observed on Mars.

The distribution and behavior of Martian ground ice during past and present epochs

Mars undergoes significant oscillations in its orbit, which will have a pronounced effect on its climate and, in particular, on the behavior of subsurface water ice. We explore and map the behavior

Evidence for recent groundwater seepage and surface runoff on Mars.

TLDR
Gullies within the walls of a very small number of impact craters, south polar pits, and two of the larger martian valleys display geomorphic features that can be explained by processes associated with groundwater seepage and surface runoff.

Mars: Nature and evolution of young latitude‐dependent water‐ice‐rich mantle

High‐resolution altimetry and imaging have revealed the presence of a meters‐thick sedimentary layer at middle to high northern and southern latitudes presently covering at least 23% of the planet.
...