Formation of Martian araneiforms by gas‐driven erosion of granular material

Villiers, Simon de; Nermoen, Anders; Jamtveit, Bjørn; Mathiesen, Joachim; Meakin, Paul; Werner, Stéphanie C.

doi:10.1029/2012gl052226

Cited by 21 publications

(12 citation statements)

References 17 publications

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“…Most volunteers contribute a few classifications of Planet Four tiles before leaving the site. This is a typical response for web-based projects [Crowston and Fagnot, 2008;Zachte, 2012] and is similar to the volunteer behavior found on other Zooniverse projects [Sauermann and Franzoni, 2015]. Figure a shows the combined distribution tallied together for both logged-in and non-logged in sessions.…”

Section: User Statisticssupporting

confidence: 70%

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Planet Four: Probing springtime winds on Mars by mapping the southern polar CO2 jet deposits

Aye

Schwamb

Portyankina

et al. 2019

Icarus

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Section: User Statisticssupporting

confidence: 70%

“…3. Trapped gas escapes through ruptures in the ice, eroding and entraining material from the surface below [de Villiers et al, 2012].…”

Section: Introductionmentioning

confidence: 99%

Planet Four: Probing springtime winds on Mars by mapping the southern polar CO2 jet deposits

Aye

Schwamb

Portyankina

et al. 2019

Icarus

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“…The coincidence of the asymmetric arrangement of the striations on the same side of Baghdad Sulcus and azimuthal orientation as jet 027 suggests that these features are scour marks or dust trails. They are reminiscent of araneiform features or "spiders" on Mars (de Villiers et al 2012) which are erosional features that form in granular material from the rapid outflow of CO 2 gas through Figure 19. Histograms of nearest-neighbor geyser spacing for all geysers excluding those on Alexandria Sulcus (see Table 14).…”

Section: Geyser-sculpted Morphologymentioning

confidence: 99%

Enceladus’ Geysers: Relation to Geological Features

Helfenstein

Porco

2015

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We apply histogram analysis, photogeological methods, and tidal stress modeling to Porco et al.ʼs survey of 101 Enceladus South Polar Basin geysers and their three-dimensional orientations to test if the jet azimuths are influenced by their placement relative to surface morphology and tectonic structures. Geysers emplaced along the three most active tiger stripe fractures (Damascus Sulcus, Baghdad Sulcus, and Cairo Sulcus) occur in local groupings with relatively uniform nearest-neighbor separation distances (∼5 km). Their placement may be controlled by uniformly spaced en echelon Riedel-type shear cracks originating from left-lateral strike-slip fault motion inferred to occur along tiger stripes. The spacing would imply a lithosphere thickness of ∼5 km in the vicinity of the tiger stripes. The orientations of tilted geyser jets are not randomly distributed; rather their azimuths correlate with the directions either of tiger stripes, cross-cutting fractures, or else fine-scale local tectonic fabrics. Diurnal tidal stress modeling suggests that periodic changes of plume activity are significantly affected by crosscutting fractures that open and close at different times than the tiger stripes that they intersect. We find evidence of sub-kilometer scale morphological modification of surface geological features surrounding geysers from sublimation-aided erosion, and ablation, and scouring. We propose that the simultaneous crushing and shearing action of periodic transpressional tidal stress on ice condensing on the inside walls of geyser conduits is the mechanism that extrudes the peculiar, paired narrow ridges known as "shark fins" that flank the medial tiger stripe fissures. We present a gallery of high-resolution image mosaics showing the placement of all the jets in their source region and consequently their geological context.

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“…It's worth to note here that formation of araneiform patterns was investigated under laboratory settings by de Villiers et al (2012). The authors simulated a transient air over-pressure above and within the granular medium of spherical silicate glass beads using Hele-Shaw cell set-up.…”

Section: Introduction: Araneiforms and Cold Jet Erosionmentioning

confidence: 99%

How martian araneiforms get their shapes: morphological analysis and diffusion-limited aggregation model for polar surface erosion

Portyankina

Hansen

Aye

2020

Icarus

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Araneiforms are radially converging systems of branching troughs exhibiting fractal properties. They are found exclusively in the Southern polar regions of Mars and believed to be result of multiple repetitions of cold CO 2 gas jets eruptions. Araneiform troughs get carved by the overpressurized gas rushing underneath a seasonal ice layer towards a newly created opening. Current work is an attempt to quantitatively analyze araneiforms patterns and model their formation mechanism. Araneiform shapes range from small and simple structures of one or two connected branches to intricate dendritic patterns several kilometers across. The dendritic quality of most araneiforms are suggestive that they can be described in terms commonly applied to terrestrial rivers. The main difference between rivers and araneiforms from the morphological point of view is that araneiform patterns are not directed or in any way influenced by the local gravitational gradient. We have adapted and for the first time applied to Martian araneiforms qualitative morphological analysis typically used for terrestrial rivers. For several locations in the Martian Southern polar regions we have calculated the largest order of tributaries, tributary densities, and bifurcation ratios. We have shown that the large and well-developed araneiforms (with tributary orders larger than 4) closely follow Horton's law of tributary orders and have bifurcation ratio that falls well inside the range of terrestrial rivers. We have implemented a two-dimensional Diffusion-Limited Aggregation (DLA) model that describes formation of dendrite shapes by mathematical probabilistic means. We compared modeled dendrite shapes to the araneiform shapes observed in the Martian polar regions and evaluated their similarity using the morphological

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Formation of Martian araneiforms by gas‐driven erosion of granular material

Cited by 21 publications

References 17 publications

Planet Four: Probing springtime winds on Mars by mapping the southern polar CO2 jet deposits

Planet Four: Probing springtime winds on Mars by mapping the southern polar CO2 jet deposits

Enceladus’ Geysers: Relation to Geological Features

How martian araneiforms get their shapes: morphological analysis and diffusion-limited aggregation model for polar surface erosion

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