Ice in channels and ice-rock mixtures in valleys on Mars
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Ice in channels and ice-rock mixtures in valleys on Mars did they slide on deformable rubble like Antarctic ice streams?

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English

Subjects:

  • Ice.,
  • Mars (Planet),
  • Mars surface.,
  • Deformation.,
  • Ross ice shelf.

Book details:

Edition Notes

Other titlesIce in channels and ice rock mixtures in valleys on Mars., Did they slide on deformable rubble like Antarctic ice streams?
StatementB.K. Lucchitta.
Series[NASA contractor report] -- NASA/CR-97-207702., NASA contractor report -- NASA CR-207702.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL18122068M

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Get this from a library! Ice in channels and ice-rock mixtures in valleys on Mars: did they slide on deformable rubble like Antarctic ice streams?. [Baerbel K Lucchitta; United States. National Aeronautics and Space Administration.]. These features include lobate debris aprons, concentric crater fill and lineated valley fill. The lateral extent of these rock glaciers can range from 5 km to over 20 km. A simple time-marching model is developed and used here to demonstrate the ability of ice and ice-rock mixtures to Cited by: Here, deformation experiments have been carried out on polycrystalline samples of pure ice, ice–rock and D2O-ice–rock mixtures at temperatures of , and K, confining pressure of 0. Flow-like features in Valles Marineris, Mars: possible ice-driven creep processes. The distribution and amount of ground ice on Mars is an important issue for the future exploration of this.

Did ice streams shape the largest channels on Mars? Edwin S. Kite1,2 and Richard C. A. Hindmarsh3 Received 29 April ; revised 7 July ; accepted 10 August ; published 3 October [1] The largest channels on Mars are the Northwestern Slope Valleys (NSVs) of Tharsis, which have previously been interpreted as the probable erosional.   Scientists have discovered large sections of underlying water ice on Mars, opening new possibilities for future exploration of the Friday’s issue of journal Science, a team of researchers led by U.S. Geological Survey planet geologist Colin Dundas have presented eight Martian regions where erosion has : Lawrence Arboleda. The planet Mars has two permanent polar ice caps. During a pole's winter, it lies in continuous darkness, chilling the surface and causing the deposition of 25–30% of the atmosphere into slabs of CO2 ice. When the poles are again exposed to sunlight, the frozen CO2 sublimes. These seasonal actions transport large amounts of dust and water vapor, giving rise to Earth-like frost and large cirrus clouds. .   The light detection and ranging instrument on the Phoenix mission observed water-ice clouds in the atmosphere of Mars that were similar to cirrus clouds on Earth. Fall streaks in the cloud structure traced the precipitation of ice crystals toward the ground. Measurements of atmospheric dust indicated that the planetary boundary layer (PBL) on Mars was well mixed, up to heights of around 4.

Mars had outgassed at least to 1 km of water, 10 to 20 bar of CO 2, and to bar of N volatiles that have been retained are mostly in the cratered uplands. Terrain softening, fretted channels, debris flows, and closed depressions indicate that at least the upper 2 km of the cratered uplands at high latitudes (>30°) contain ice in amounts that exceed the porosity, estimated to Cited by:   Lobate debris aprons are landforms observed in the mid-latitudes regions of Mars at the foot of kilometer high scarps. Because of their lobate front and convex shape they have been interpreted as the result of the viscous deformation of an ice-rock mixture. Recent analyses of Mars Observer Laser Altimeter (MOLA) data confirm these previous conclusions. Fretted channels correspond to lineated Cited by: 4. Lineated valley fill (LVF), also called lineated floor deposit, is a feature of the floors of some channels on Mars, exhibiting ridges and grooves that seem to flow around obstacles. Shadow measurements show that at least some of the ridges are several metres high. LVF is believed to be ice-rich. The rate of abrasion initially increases as glacial pressure and ice velocity increase, but decreases as the pressure becomes too great and ice at the base of the glacier begins to melt and release rock fragments from ice-rock fragment mixture. Abrasion increases with the increase in basal debris concentration.