The geology of the Viking Lander 2 site

Mutch, Thomas A.; Arvidson, R. E.; Binder, A. B.; Guinness, E. A.; Morris, E. C.

doi:10.1029/js082i028p04452

Cited by 181 publications

(109 citation statements)

References 22 publications

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“…The rocks of this type are typically not lying on the surface but appear to be almost completely (Scooby Doo) or partially buried (Casper). The morphology of this unit is consistent with a chemically bonded crust or hardpan, similar to that reported at the VL-2 site (32). Digging tests with the rover wheels failed to dislodge any material from Scooby Doo, indicating at least a partially cemented or highly compacted material.…”

supporting

confidence: 62%

Results from the Mars Pathfinder Camera

Smith

Bell

Bridges

et al. 1997

Science

237

151

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supporting

confidence: 62%

Results from the Mars Pathfinder Camera

Smith

Bell

Bridges

et al. 1997

Science

237

151

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“…The crusty-to-cloddy material was similar to the blocky material in that it appeared to consist of cemented grains of finer material but seemed more consolidated. The overall conclusion that was reached at the time of the Viking landings was that the geological processes that were identified from orbiter images could not be identified uniquely from lander images [Masursky and Crabill, 1976a,b;Binder et al, 1977;Mutch et al, 1977]. That is, the processes that were responsible for the 100-m-scale features were not necessarily the same as those that were responsible for the decimeter-and meterscale features.…”

Section: Geology Of the Viking Landing Sitesmentioning

confidence: 99%

High‐resolution thermal inertia mapping of Mars: Sites of exobiological interest

Jakosky¹,

Mellon²

2001

J. Geophys. Res.

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Abstract. We have mapped thermal inertia at high resolution for selected regions of Mars that are of potential biological relevance, using observations made by the Mars Global Surveyor Thermal Emission Spectrometer. Thermal inertia is a direct indicator of physical properties of the surface at the decimeter-to-meter scale. Our goal is to understand the geological processes by which the sites formed and their subsequent evolution, their current state, and their safety and science potential as landing sites for future lander, rover, and sample-return spacecraft missions. The thermal inertia values at -3-km scale for the sites considered span the entire range of values measured at Mars; thermal inertias range from low values indicative of substantial aeolian mantling up to high values suggesting surfaces covered predominantly with bedrock, exposed rocks or blocks, or wellindurated crusts. The highest thermal inertias correlate strongly with local morphology, while areas with intermediate and low thermal inertias generally show no such correlation. This suggests that selection of future landing sites will be plagued by a choice of a well-mantled site that is safe but less interesting scientifically versus an unmantied site that is more interesting scientifically but less safe.

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“…The surface features on these rocks have been generally interpreted as volcanic vesicles only slightly modified by wind action Mutch et al, 1977]. Some of the rocks do appear to contain irregularly shaped but closely spaced pits with overhanging external canopies.…”

Section: Viking Comparisonsmentioning

confidence: 99%

Pitted and fluted rocks in the western desert of Egypt: Viking comparisons

McCauley

Breed²,

El-Baz

et al. 1979

J. Geophys. Res.

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The Western Desert of Egypt is one of the most arid regions on Earth and is probably our closest terrestrial analog to the surface of Mars. An expedition to the area in 1978 revealed an abundance of quartzite and basalt rocks that have been pitted and fluted by wind erosion and deflation of the desert surface. These pitted rocks are internally homogeneous, show no internal holes or vesicles, and are considered an important but neglected type of ventifact. They bear a striking resemblance to the pitted and fluted rocks seen by the Viking Landers, rocks that have generally been interpreted as vesicular basalts only slightly modified by wind erosion. Wind tunnel studies of the air flow over and around nonstreamlined hand specimens from the Western Desert show that windward abrasion coupled with negative flow, secondary flow, and vorticity in a unidirectional wind can explain the complex arrays of pits and flutes. These field and laboratory observations suggest that the pitted rocks at the Viking Lander sites are also ventifacts, and thus the Martian surface may be far more wind eroded than previously thought.

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The geology of the Viking Lander 2 site

Cited by 181 publications

References 22 publications

Results from the Mars Pathfinder Camera

Results from the Mars Pathfinder Camera

High‐resolution thermal inertia mapping of Mars: Sites of exobiological interest

Pitted and fluted rocks in the western desert of Egypt: Viking comparisons

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