Possible pingos and a periglacial landscape in northwest Utopia Planitia

Soare, R. J.; Burr, D. M.; Tseung, J. M. Wan Bun

doi:10.1016/j.icarus.2004.11.013

Cited by 84 publications

(43 citation statements)

References 35 publications

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“…and our previous studies (Ulrich et al, 2010). Furthermore, various periglacial-like features have been observed in the region, e.g., polygonal structures, scalloped depressions, and small mounds (e.g., Soare et al, 2005;Morgenstern et al, 2007;Burr et al, 2009;de Pablo and Komatsu, 2009;Lefort et al, 2009;Levy et al, 2009b;Ulrich et al, 2010;Séjourné et al, 2011). These landforms are associated in a geomorphological context, suggesting the existence of ice-rich ground (e.g., Morgenstern et al, 2007;Lefort et al, 2009;Ulrich et al, 2010).…”

Section: Mars (Utopia Planitia Up)supporting

confidence: 58%

Polygon pattern geomorphometry on Svalbard (Norway) and western Utopia Planitia (Mars) using high-resolution stereo remote-sensing data

et al. 2011

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Polygonal systems formed by thermal contraction cracking are complex landscape features widespread in terrestrial periglacial regions. The manner in which cracking occurs is controlled by various environmental factors and determines dimension, shape, and orientation of polygons. Analogous small-scale features are ubiquitous in Martian mid-and high-latitudes, and they are also inferred to originate from thermal contraction cracking. We studied the geomorphometry of polygonally-patterned ground on Svalbard to draw a terrestrial analogy to small-scale polygonal structures in scalloped terrain in Martian mid-latitudes. We performed a comparative quantitative terrain analysis based on high-resolution stereo remote-sensing data (HRSC-AX and HiRISE) in combination with terrestrial field data and multivariate statistics to determine the relationship of polygon geomorphometry to local environmental conditions. Results show that polygonal structures on Svalbard and in Utopia Planitia on Mars are similar with respect to their size and shape. A comparable thermal contraction cracking genesis is likely. Polygon evolution, however, is strongly related to regional and local landscape dynamics. Individual polygon dimensions and orthogonality vary according to age, thermal contraction cracking activity, and local subsurface conditions. Based on these findings, the effects of specific past and current environmental conditions on polygon formation on Mars must be considered. On both Earth and Mars, the smallest polygons represent young, recently-active low-centered polygons that formed in fine-grained ice-rich material. Small, low-centered Martian polygons show the closest analogy to terrestrial low-centered ice-wedge polygons. The formation of composite wedges could have occurred as a result of local geomorphological conditions during past Martian orbital configurations. Larger polygons reflect past climate conditions on both Earth and Mars. The present degradation of these polygons depends on relief and topographical situation. On Svalbard the thawing of ice wedges degrades high-centered polygons; in contrast, the present appearance of polygons in Utopia Planitia is primarily the result of contemporary dry degradation processes.

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Section: Mars (Utopia Planitia Up)supporting

confidence: 58%

Polygon pattern geomorphometry on Svalbard (Norway) and western Utopia Planitia (Mars) using high-resolution stereo remote-sensing data

et al. 2011

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“…Pingo-like features (PLFs) also occur in extraterrestrial, periglacial environments such as on Mars (Cabrol et al, 2000;Burr et al, 2005Burr et al, , 2009Soare et al, 2005). Proof of the existence of Martian pingo analogs may indicate presence of massive ground ice and subsurface water flow on Mars in the past.…”

Section: Pingo Database Applicationsmentioning

confidence: 99%

Assessment of pingo distribution and morphometry using an IfSAR derived digital surface model, western Arctic Coastal Plain, Northern Alaska

et al. 2012

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“…In addition, over the past ∼20 Ma, Mars' obliquity has periodically varied by several tens of degrees with a period of a few tens of thousands of years (Laskar et al, 2004), and thus ice is likely to have also been periodically stably deposited at mid-latitudes for substantial periods over this time (Chamberlain and Boynton, 2007;Mischna et al, 2003). Mid-latitude landforms such as polygonal patterned ground, shallow pits, and pitted mounds and cones (ring-mound landforms; Jaeger et al, 2007) have also therefore been ascribed to periglacial processes (Dundas et al, 2008;Soare et al, 2005). Climate model results suggest that ice could be stable even near the equator if obliquity was as high as 45 • (as might have occurred about 5 Ma before present; Laskar et al, 2004), but only at high elevations (Forget et al, 2006), in agreement with observations of glacial landforms seen on the flanks of large martian volcanoes (Head and Marchant, 2003).…”

Section: Introductionmentioning

confidence: 99%

Sorted stone circles in Elysium Planitia, Mars: Implications for recent martian climate

Balme

Gallagher

Page

et al. 2009

Icarus

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Possible pingos and a periglacial landscape in northwest Utopia Planitia

Cited by 84 publications

References 35 publications

Polygon pattern geomorphometry on Svalbard (Norway) and western Utopia Planitia (Mars) using high-resolution stereo remote-sensing data

Polygon pattern geomorphometry on Svalbard (Norway) and western Utopia Planitia (Mars) using high-resolution stereo remote-sensing data

Assessment of pingo distribution and morphometry using an IfSAR derived digital surface model, western Arctic Coastal Plain, Northern Alaska

Sorted stone circles in Elysium Planitia, Mars: Implications for recent martian climate

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