Earth-like sand fluxes on Mars

Bridges, N. T.; Ayoub, F.; Avouac, Jean Philippe; Leprince, S.; Lucas, Antoine; Mattson, S.

doi:10.1038/nature11022

Cited by 236 publications

(308 citation statements)

References 27 publications

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“…The sand flux measured over a 3-month period in the northern winter of MY28 (2007) (ref. 10) is comparable, though about 30% lower, to the winter values obtained for MY30 in this study. We measure only the space-and time-averaged values within each period separating each data acquisition, although a glimpse of the stochasticity of sand-moving winds can be inferred, as follows.…”

Section: Resultssupporting

confidence: 79%

“…Using this estimated DEM error, we estimated its contribution on all the migration maps by taking into account the stereoscopic angle between each image pairs of the time series. Ripple migration linearly scales with the elevation of the dune 10 , such that the error in elevation will linearly scale with the dune elevation. We estimate the maximum, average and s.d.…”

Section: Methodsmentioning

confidence: 99%

“…In the meantime, dunes migrate, such that using a unique DEM may cause a misalignment of dunes with the images. In Bridges et al 10 , dune migration speed was estimated to B1 m per year for the fastest dunes. According to the DEM, the slopes of the dunes' stoss slopes in the 'axial' direction are 4-8°.…”

Section: Methodsmentioning

confidence: 99%

“…Aeolian processes are known to dominate the current Martian climate through the modulation of atmospheric thermal forcing by suspended dust [3][4][5][6] . However, the intensity of wind activity has been judged as significantly lower than on Earth, such that recent evidence for currently active dune migration [7][8][9] and measurements of Martian sand fluxes comparable to terrestrial values 10 came as a surprise. Prevailing expectations based on wind tunnel experiments, theory for initiation of saltation, atmospheric modelling and limited in situ wind measurements suggested that sand-moving winds should be very rare [11][12][13][14][15][16] .…”

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confidence: 99%

“…The apparent contradiction between rare implied saltation and reasonably common dust lifting 17,18 remains unresolved but has variously been ascribed to the uncertainties in interparticle cohesion, the role of electrostatics, the role of gustiness and the vertical wind shear and suction in dust devils 18,19 . Indeed, a major dust storm occurred during the time period between the acquisitions of the two images analyzed in the preceding Nili Patera High Resolution Imaging Science Experiment (HiRISE) study 10,20 , allowing the possibility that anomalously high storm winds accounted for a significant fraction of the measured sand flux.…”

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confidence: 99%

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Threshold for sand mobility on Mars calibrated from seasonal variations of sand flux

et al. 2014

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Coupling between surface winds and saltation is a fundamental factor governing geological activity and climate on Mars. Saltation of sand is crucial for both erosion of the surface and dust lifting into the atmosphere. Wind tunnel experiments along with measurements from surface meteorology stations and modelling of wind speeds suggest that winds should only rarely move sand on Mars. However, evidence for currently active dune migration has recently accumulated. Crucially, the frequency of sand-moving events and the implied threshold wind stresses for saltation have remained unknown. Here we present detailed measurements of Nili Patera dune field based on High Resolution Imaging Science Experiment images, demonstrating that sand motion occurs daily throughout much of the year and that the resulting sand flux is strongly seasonal. Analysis of the seasonal sand flux variation suggests an effective threshold for sand motion for application to large-scale model wind fields (1-100 km scale) of t s ¼ 0.01±0.0015 N m À 2 .

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Section: Resultssupporting

confidence: 79%

Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

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confidence: 99%

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confidence: 99%

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Threshold for sand mobility on Mars calibrated from seasonal variations of sand flux

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Sands at Gusev Crater, Mars

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Herkenhoff

Knoll

et al. 2014

J. Geophys. Res. Planets

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Processes, environments, and the energy associated with the transport and deposition of sand at Gusev Crater are characterized at the microscopic scale through the comparison of statistical moments for particle size and shape distributions. Bivariate and factor analyses define distinct textural groups at 51 sites along the traverse completed by the Spirit rover as it crossed the plains and went into the Columbia Hills. Fine-to-medium sand is ubiquitous in ripples and wind drifts. Most distributions show excess fine material, consistent with a predominance of wind erosion over the last 3.8 billion years. Negative skewness at West Valley is explained by the removal of fine sand during active erosion, or alternatively, by excess accumulation of coarse sand from a local source. The coarse to very coarse sand particles of ripple armors in the basaltic plains have a unique combination of size and shape. Their distribution display significant changes in their statistical moments within the~400 m that separate the Columbia Memorial Station from Bonneville Crater. Results are consistent with aeolian and/or impact deposition, while the elongated and rounded shape of the grains forming the ripples, as well as their direction of origin, could point to Ma'adim Vallis as a possible source. For smaller particles on the traverse, our findings confirm that aeolian processes have dominated over impact and other processes to produce sands with the observed size and shape patterns across a spectrum of geologic (e.g., ripples and plains soils) and aerographic settings (e.g., wind shadows).

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The rock abrasion record at Gale Crater: Mars Science Laboratory results from Bradbury Landing to Rocknest

et al. 2014

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Ventifacts, rocks abraded by wind-borne particles, are found in Gale Crater, Mars. In the eastward drive from "Bradbury Landing" to "Rocknest," they account for about half of the float and outcrop seen by Curiosity's cameras. Many are faceted and exhibit abrasion textures found at a range of scales, from submillimeter lineations to centimeter-scale facets, scallops, flutes, and grooves. The drive path geometry in the first 100 sols of the mission emphasized the identification of abrasion facets and textures formed by westerly flow. This upwind direction is inconsistent with predictions based on models and the orientation of regional dunes, suggesting that these ventifact features formed from very rare high-speed winds. The absence of active sand and evidence for deflation in the area indicates that most of the ventifacts are fossil features experiencing little abrasion today.

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Earth-like sand fluxes on Mars

Cited by 236 publications

References 27 publications

Threshold for sand mobility on Mars calibrated from seasonal variations of sand flux

Threshold for sand mobility on Mars calibrated from seasonal variations of sand flux

Sands at Gusev Crater, Mars

The rock abrasion record at Gale Crater: Mars Science Laboratory results from Bradbury Landing to Rocknest

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