Permafrost features on the martian surface

Wade, F. Alton; Wys, J. Negus de

doi:10.1016/0019-1035(68)90011-0

Cited by 27 publications

(9 citation statements)

References 13 publications

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“…These potential alteration scenarios are built upon observations of Mars and evidence for water, condensates, dust and duricrust on the surface. Early studies of Mars suggested the possibility of water and/or ice on the surface [ Salisbury , 1966; Anderson et al , 1967; Wade and de Wys , 1968; Masursky , 1973; Baker and Milton , 1974]. Analysis of the channels in Viking images led Masursky et al [1977] and Carr [1979] to suggest the possibility of fluvial activity.…”

Section: Introductionmentioning

confidence: 99%

A model for formation of dust, soil, and rock coatings on Mars: Physical and chemical processes on the Martian surface

et al. 2002

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[1] A model is presented here to explain the generation of surface material on Mars using chemical, magnetic, and spectroscopic data from Mars and geologic analogs from terrestrial sites. One basic premise is that the dust/soil units are not derived exclusively from local rocks, but are rather a product of global, and possibly remote, weathering processes. Another assumption in this model is that there are both physical and chemical interactions of the atmosphere with dust particles and that these two processes create distinctly different products. Physical processes distribute dust particles on rocks and drift units, forming physically aggregated layers; these are reversible processes. Chemical reactions of the dust/soil particles create alteration rinds on rock surfaces and cohesive, crusted surface units between rocks, both of which are relatively permanent materials. According to this model the dominant components of the dust/soil particles are derived from alteration of volcanic ash and tephra and contain primarily nanophase and poorly crystalline ferric oxide/oxyhydroxide phases as well as silicates. These phases are the alteration products that formed in a low-moisture environment. These dust/soil particles also contain a smaller amount of material that was exposed to more water and contains crystalline ferric oxides/oxyhydroxides, sulfates, and clay silicates. These components could have formed through hydrothermal alteration at steam vents or fumeroles, thermal fluids, or through evaporite deposits. Wet/dry cycling experiments are presented here on Mars soil analogue mixtures containing poorly crystalline and crystalline components dominated by nanophase to $2 mm diameter particles. Cemented products of these soil mixtures are formed in these experiments, and variation in the surface texture was observed for samples containing smectites, nonhydrated silicates, or sulfates. Reflectance spectra were measured of the initial particulate mixtures, the cemented products, and ground versions of the cemented material. The spectral contrast in the visible/near-infrared and midinfrared regions is significantly reduced for the cemented material compared to the initial soil and somewhat reduced for the ground, cemented soil compared to the initial soil. The results of this study suggest that transient fluvial activity on Mars will have a profound effect on the texture and spectral properties of the dust/soil particles on the surface. The model developed in this study provides an explanation for the generation of cemented or crusted soil units and rock coatings on Mars and may explain albedo variations on the surface observed near large rocks or crater rims.

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Section: Introductionmentioning

confidence: 99%

A model for formation of dust, soil, and rock coatings on Mars: Physical and chemical processes on the Martian surface

et al. 2002

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“…The presence of permafrost on Mars was suspected even before quality imagery was obtained of the planet's surface (Anderson et al, 1967;Wade and deWys, 1968). Following the success of the Mariner 9 Mission, many analogies were suggested between terrestrial and Martian cold-climate terrains (Anderson et al, 1972;Gatto and Anderson, 1975;Sharp, 1973d).…”

Section: Periglacial and Permafrost Featuresmentioning

confidence: 97%

The geomorphology of Mars

Baker¹

1981

Progress in Physical Geography: Earth and Environment

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“…Positive relief fillings result after mud crack formation when the mud cracks are filled with sand deposited by wind or the next lake filling. If polygonal features 10 to 30 m in diameter are detected they are probably not mud cracks but are sand wedge formations in permafrost soil [ Wade and De Wys , 1968; Mellon , 1997]. Freeze/thaw cycles of a soil with significant frozen water must occur for sand wedge polygons to form.…”

Section: Geologic and Pedogenic Hypothesesmentioning

confidence: 99%

Examining the sediments and soils of Gusev Crater with the Athena science payload

2004

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[1] Gusev Crater has been proposed to contain lacustrine and/or fluvial sediments; however, eolian or volcanic sediments, global dust, and locally produced soils may also be present. This work describes the use of the Athena instrument package to evaluate the environment in which sampled materials were deposited in Gusev Crater. Sedimentary or soil deposits can be sampled by examining materials that were (1) excavated by impact events, (2) revealed by wind deflation, or (3) exposed by spinning the rover wheels. Specific observations can be diagnostic of a depositional environment. For instance, Pancam images of thin (e.g., 5 cm) planar layers of phyllosilicates and/or evaporites (as determined by Mini-TES) would suggest lacustrine sediments. Layered sediments (e.g., trough cross bed) with rounded particles (>4 mm) would suggest fluvial activity. Eolian sediments may have planar or cross-planar layers of well-sorted grains ($200 mm). Parallel bed deposits consisting of glass observable by Microscopic Imager would indicate volcanic ash. Soil bulk chemistry reported by Alpha Particle X-ray Spectrometer that is similar to the Viking and Mars Pathfinder soils would indicate global dust. Mini-TES should only detect primary mineralogies in physically weathered soils, whereas chemically weathered soils may contain carbonates, sulfates, and/or phyllosilicates. Although some characteristics are unique to a sediment or soil deposit, different deposit types can have similar characteristics (e.g., planar layering). Determining the depositional history of material in Gusev will require the integration of measurements from several instruments and careful geologic reasoning by the investigators.

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Permafrost features on the martian surface

Cited by 27 publications

References 13 publications

A model for formation of dust, soil, and rock coatings on Mars: Physical and chemical processes on the Martian surface

A model for formation of dust, soil, and rock coatings on Mars: Physical and chemical processes on the Martian surface

The geomorphology of Mars

Examining the sediments and soils of Gusev Crater with the Athena science payload

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