Co-evolution of polygonal and scalloped terrains, southwestern Utopia Planitia, Mars

Haltigin, T. W.; Pollard, W. H.; Dutilleul, Pierre; Osinski, G. R.; Koponen, L.

doi:10.1016/j.epsl.2013.11.005

Cited by 8 publications

(5 citation statements)

References 62 publications

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“…On Mars, Oehler and Allen () proposed polygonal faulting as a mechanism to explain ∼2‐ to 10‐km polygons expressed on the surface of Acidalia and Utopia Planitia, using this to argue for their formation in a subaqueous setting. Similar features have also been attributed to periglacial processes (e.g., Haltigin et al, ). Unlike these examples, the northeast Syrtis layered sulfates show the full 3‐D geometry of the fault network, which allows a much clearer identification of polygonal faulting, since the ridge characteristics match the scale, morphology, and penetrative nature of the fractures.…”

Section: Discussionsupporting

confidence: 75%

The Deposition and Alteration History of the Northeast Syrtis Major Layered Sulfates

Quinn

Ehlmann

2019

JGR Planets

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Ancient stratigraphy on Isidis Basin's western margin records the history of water on early Mars. Noachian units are overlain by layered, basaltic composition sedimentary rocks that are enriched in polyhydrated sulfates and capped by more resistant units. The layered sulfates—uniquely exposed at northeast Syrtis Major—comprise a sedimentary sequence up to 600 m thick that has undergone a multistage history of deposition, alteration, and erosion. Siliciclastic sediments enriched in polyhydrated sulfates are bedded at meter scale and were deposited on slopes up to 10°, embaying and thinning against preexisting Noachian highlands around the Isidis Basin rim. The layered sulfates were modified by volume loss fracturing during diagenesis. Resultant fractures hosted channelized flow and jarosite mineral precipitation to form resistant ridges upon erosion. The structural form of the layered sulfates is consistent with packages of sediment fallen from either atmospheric or aqueous suspension; coupling with substantial diagenetic volume loss may favor deepwater basin sedimentation. After formation, the layered sulfates were capped by a “smooth capping unit” and then eroded to form paleovalleys. Hesperian Syrtis Major lavas were channelized by this paleotopography, capping it in some places and filling it in others. Later fluvial features and phyllosilicate‐bearing lacustrine deposits, sharing a regional base level of ∼−2,300 m, were superimposed on the sulfate‐lava stratigraphy. The layered sulfates suggest surface bodies of water and active groundwater upwelling during the Noachian‐Hesperian transition. The northeast Syrtis Major stratigraphy records at least four distinct phases of surface and subsurface aqueous activity spanning from late Noachian to early Amazonian time.

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Section: Discussionsupporting

confidence: 75%

The Deposition and Alteration History of the Northeast Syrtis Major Layered Sulfates

Quinn

Ehlmann

2019

JGR Planets

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“…On a given slope polygon dimensions should be larger for a deeper ice table (Mellon et al, 2008a), but small polygons might remain visible as the ice retreats, especially if the lag eventually becomes thick enough to inhibit cracking. Haltigin et al (2014) reported that at the landscape scale, polygons in Utopia are systematically smaller in lower-elevation areas, and also noted dramatically higher polygon densities at the base of scallop scarps. One possible factor is that the hectometer-scale inter-scallop polygons of Utopia Planitia may not be of seasonal thermal contraction origin, but instead relate to deformation of a thin surface layer (Yoshikawa, 2003), which could equate to the ice-rich surface unit inferred by Stuurman et al (2014).…”

Section: Scalloped Depressionsmentioning

confidence: 97%

“…One possibility is that this reflects primarily eolian erosion of the regolith on the steep slope, as suggested by Lefort et al (2009) for pole-oriented scallops. Haltigin et al (2014) suggested that wind could enhance sublimation on pole-facing scarps, but for thick lags the rate of sublimation will be controlled by diffusion. For very shallow ice, however, free and forced convection of water vapor should control sublimation rates.…”

Section: Sublimation Thermokarst On Marsmentioning

confidence: 99%

Modeling the development of martian sublimation thermokarst landforms

Dundas¹,

Byrne²,

McEwen³

2015

Icarus

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a b s t r a c tSublimation-thermokarst landforms result from collapse of the surface when ice is lost from the subsurface. On Mars, scalloped landforms with scales of decameters to kilometers are observed in the midlatitudes and considered likely thermokarst features. We describe a landscape evolution model that couples diffusive mass movement and subsurface ice loss due to sublimation. Over periods of tens of thousands of Mars years under conditions similar to the present, the model produces scallop-like features similar to those on the martian surface, starting from much smaller initial disturbances. The model also indicates crater expansion when impacts occur in surfaces underlain by excess ice to some depth, with morphologies similar to observed landforms on the martian northern plains. In order to produce these landforms by sublimation, substantial quantities of excess ice are required, at least comparable to the vertical extent of the landform, and such ice must remain in adjacent terrain to support the nondeflated surface. We suggest that martian thermokarst features are consistent with formation by sublimation, without melting, and that significant thicknesses of very clean excess ice (up to many tens of meters, the depth of some scalloped depressions) are locally present in the martian mid-latitudes. Climate conditions leading to melting at significant depth are not required.Published by Elsevier Inc.http://dx.

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“…Polygonal features on Mars can develop in various scales and geological settings. For example, polygons of 5–15 m in diameter have been observed in Athabasca Valles and are considered to be formed by contraction during lava cooling (Ryan & Christensen, 2012); possible ice‐wedge polygons formed by freeze‐thaw cycling are widely distributed in middle latitudes of Utopia Planitia and Argyre Basin (Soare et al., 2014, 2021); thermal contraction of ice‐rich permafrost also formed meter‐sized polygons across Martian middle to high latitudes (Haltigin et al., 2014; Levy et al., 2009); polygonal features ranging from several meters to hundreds of meters in size with a desiccation origin have been identified in local lows with chloride or clay‐rich deposits (Dang et al., 2020; El Maarry et al., 2010; Ye et al., 2019); large‐scale (several to tens of kilometers in size) polygonal terrains are widely distributed in the Utopia Planitia and could be related to volumetric compaction of sedimentary deposits in the Utopia Basin (Buczkowski et al., 2012). In addition, in situ investigations by the Opportunity rover identified centimeter‐ to decimeter‐scale polygons in sedimentary layers and they are considered as contractional cracks (Grotzinger et al., 2006; McLennan et al., 2005).…”

Section: Discussionmentioning

confidence: 99%

Recent Aqueous Activity on Mars Evidenced by Transverse Aeolian Ridges in the Zhurong Exploration Region of Utopia Planitia

Wang

Zhao

Xiao

et al. 2023

Geophysical Research Letters

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Aqueous activities on Mars have gradually declined since the Noachian (>3.7 Ga). Although water can be stored in the subsurface during the latest epochs, geomorphological evidence is still limited. In this study, we used in situ imaging and spectral data acquired by China's Zhurong rover, as well as high-resolution remote-sensing data, to investigate the transverse aeolian ridges (TARs) in the Zhurong landing region of Utopia Planitia. A two-stage evolutionary scenario of the TARs is proposed and polygonal features with hydrated minerals are identified for the first time on the surface of Martian TARs. We discussed the possible formation mechanisms of the polygonal features, and proposed that they could be related to recent aqueous activity and atmosphere-surface water exchange on Mars, which sheds light on the hydrological cycle of Mars in current cold and dry climate. Plain Language SummaryThe history of water on the surface of Mars has been studied for a long time. Since about 3.7 billion years ago, the role of water has gradually declined. Although the existence of subsurface ice on present-day Mars has been confirmed, evidence for surface water is still limited. Transverse aeolian ridges (TARs), a kind of ripple-like aeolian landform, are widely distributed on Mars and usually thought to be active within the last ∼3 million years. They are also identified in southern Utopia Planitia, the landing region of China's Mars exploration rover Zhurong. We analyzed the morphology and evolution of the TARs in the Zhurong landing region, and found some polygonal features with hydrated minerals such as gypsum on the surface of the latest-formed TARs. We discussed the possible origins of these polygons, and proposed that they represent very recent aqueous activity on the Martian surface, which will help us better understand the hydrological cycle on current Mars.

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Co-evolution of polygonal and scalloped terrains, southwestern Utopia Planitia, Mars

Cited by 8 publications

References 62 publications

The Deposition and Alteration History of the Northeast Syrtis Major Layered Sulfates

The Deposition and Alteration History of the Northeast Syrtis Major Layered Sulfates

Modeling the development of martian sublimation thermokarst landforms

Recent Aqueous Activity on Mars Evidenced by Transverse Aeolian Ridges in the Zhurong Exploration Region of Utopia Planitia

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