Thermophysical Properties of Martian Fluvial Sinuous Ridges: Inferences on “Inverted Channel” Induration Agent

Williams, R. M. E.; Moersch, Jeffrey E.; Fergason, Robin L.

doi:10.1029/2018ea000402

Cited by 20 publications

(19 citation statements)

References 72 publications

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“…The chlorides from brines might work as cement and would be sufficient to enable this process, consistent with the notion of Williams et al. (2018) that fluvial channels on Mars are typically inverted due to cementation, as opposed to clast armoring or lava filling. A changed grain‐size may also have an effect on the consolidation of the material, whereby larger grains increase the resistance to erosion.…”

Section: Discussionsupporting

confidence: 84%

Geological History of Southeastern Gorgonum Chaos, Mars: A Story of Water and Wind

2021

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Gorgonum Chaos is part of the Eridania paleolake in Terra Sirenum and displays a number of prominent light-toned morphological features that bear a record of the regional climatic conditions throughout most of Martian history. Based on an intergrated analysis of orbital data, we mapped a 1500 km 2 area in the southeast of Gorgonum Chaos. Morphologic, spectroscopic and stratigraphic analyses were used to determine age and composition of the main geological units in the area. We identified four major geological units with decreasing content of hydrated minerals from the oldest to the youngest units, which were completely free of hydrated minerals. In the study area phyllosilicate-rich Noachian units compose the majority of the basin floor. Deposits enriched with evaporites were formed around the Noachian/Hesperian transition and erosion created prominent inverted morphologies. Loess-like material without significant amounts of hydrated minerals was deposited until the late Hesperian. The youngest unit is an Amazonian layer free of hydrated minerals that originated from volcanic activities. This succession of minerals reflects the transition from more humid climatic conditions with the ability to sustain liquid water on the planet's surface during the Noachian to the hyper-arid Amazonian environment we observe currently on Mars.

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Section: Discussionsupporting

confidence: 84%

Geological History of Southeastern Gorgonum Chaos, Mars: A Story of Water and Wind

2021

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“…For most occurrences of Martian inverted channels, there is not an obvious connection to a volcanic source, and therefore lava-capping is considered a relatively rare induration mechanism. Williams et al (2018) argue that the geologic setting and thermophysical characteristics of many of the larger inverted fluvial landforms on Mars are consistent with a cementation induration agent, rather than clast-armoring. With this study we document another mechanism for generating salt mineralogy associated with inverted channels; rather than cementing the fluvial deposits, chemical sedimentation was concentrated within the fluvial channel.…”

Section: Discussionmentioning

confidence: 90%

Section: Discussionmentioning

confidence: 90%

“…Two characteristics that could aid in differentiating cementation from clast armoring for Martian inverted channels are a) the time-varying thermal signature of the ridge, and b) the cross-sectional ridge shape. Preliminary studies in the Salar de Llamara show that the diurnal temperature response differs between these ridge types ( Williams et al, 2018 ), a possible criterion to distinguish the capping material on Mars in thermal images. In terms of ridge shape, the PdT gravel-capped ridge has a rounded cross-sectional form.…”

Section: Discussionmentioning

confidence: 99%

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Inverted channel variations identified on a distal portion of a bajada in the central Atacama Desert, Chile

et al. 2021

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In deserts, the interplay between occasional fluvial events and persistent aeolian erosion can form composite modern and relict surfaces, especially on the distal portion of alluvial fans. There, relief inversion of alluvial deposits by differential erosion can form longitudinal ridges. We identified two distinct ridge types formed by relief inversion on converging alluvial fans in the hyperarid Chilean Atacama Desert. Although they are co-located and similar in scale, the ridge types have different ages and formation histories that apparently correspond to minor paleoclimate variations. Gravel-armored ridges are remnants of deflated alluvial deposits with a bimodal sediment distribution (gravel and sand) dated to a minor pluvial phase at the end of the Late Pleistocene (~12 kyr). In contrast, younger (~9 kyr) sulfate-capped ridges formed during a minor arid phase with evaporite deposition in a pre-existing channel that armored the underlying deposits. Collectively, inverted channels at Salar de Llamara resulted from multiple episodes of surface overland flow and standing water spanning several thousand years. Based on ridge relief and age, the minimum long-term deflation rate is 0.1–0.2 m/kyr, driven primarily by wind erosion. This case study is an example of the equifinality concept whereby different processes lead to similar landforms. The complex history of the two ridge types can only be generally constrained in remotely sensed data. In situ observations are required to discern the specifics of the aqueous history, including the flow type, magnitude, sequence, and paleoenvironment. These findings have relevance for interpreting similar landforms on Mars.

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“…Interestingly, the thermal inertia of Aram Dorsum is low relative to the adjacent marginal unit. It could be argued that a fluvial sandstone, cemented by chemicals precipitated from a solute-rich groundwater, would have a relatively high thermal inertia, as suggested for other inverted fluvial systems on Mars (Williams et al, 2018), but this signal could represent sand or dust cover trapped in a rougher surface instead.…”

Section: Journal Of Geophysical Research: Planetsmentioning

confidence: 99%

Aram Dorsum: An Extensive Mid‐Noachian Age Fluvial Depositional System in Arabia Terra, Mars

et al. 2020

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A major debate in Mars science is the nature of the early Mars climate, and the availability of precipitation and runoff. Observations of relict erosional valley networks have been proposed as evidence for extensive surface runoff around the Noachian-Hesperian boundary. However, these valley networks only provide a time-integrated record of landscape evolution, and thus, the timing, relative timescales and intensity of aqueous activity required to erode the valleys remain unknown. Here, we investigate an ancient fluvial sedimentary system in western Arabia Terra, now preserved in positive relief. This ridge, "Aram Dorsum," is flat-topped, branching,~85 km long, and particularly well preserved. We show that Aram Dorsum was an aggradational alluvial system and that the existing ridge was once a large river channel belt set in extensive flood plains, many of which are still preserved. Smaller, palaeochannel belts feed the main system; their setting and network pattern suggest a distributed source of water. The alluvial succession is up to 60 m thick, suggesting a formation time of 10 5 to 10 7 years by analogy to Earth. Our observations are consistent with Aram Dorsum having formed by long-lived flows of water, sourced both locally, and regionally as part of a wider alluvial system in Arabia Terra. This suggests frequent or seasonal precipitation as the source of water. Correlating our observations with previous regional-scale mapping shows that Aram Dorsum formed in the mid-Noachian. Aram Dorsum is one of the oldest fluvial systems described on Mars and indicates climatic conditions that sustained surface river flows on early Mars. Plain Language SummaryThe oldest regions of Mars contain ancient valleys, carved by running water, and sinuous ridges, often interpreted as the remnants of former riverbeds, left upstanding by erosion. These "inverted channel" systems provide insight into Mars's ancient climate and hydrologic cycle. We use high-resolution satellite images to investigate "Aram Dorsum," an 85 km long ridge system in the Arabia Terra region. Our observations show that Aram Dorsum is composed of sedimentary rocks, originally deposited in rivers or their adjacent floodplains. The Aram Dorsum sedimentary material is up to 60 m thick, which, by comparison with similar sedimentary deposits on Earth, suggests that the Aram Dorsum river system was active for between 10,000 and 10 million years. Our study also indicates that Aram Dorsum was formed around 3.9 billion years ago, an age consistent with other evidence for ancient rivers and lakes in this region. The water that flowed within the rivers at Aram Dorsum probably came from both locally and regionally generated rainfall or snowfall, rather than a single point source of water, such as large distant ice sheets. Our observations therefore point to an ancient Martian climate that supported precipitation and river flow for thousands or millions of years.

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Thermophysical Properties of Martian Fluvial Sinuous Ridges: Inferences on “Inverted Channel” Induration Agent

Cited by 20 publications

References 72 publications

Geological History of Southeastern Gorgonum Chaos, Mars: A Story of Water and Wind

Geological History of Southeastern Gorgonum Chaos, Mars: A Story of Water and Wind

Inverted channel variations identified on a distal portion of a bajada in the central Atacama Desert, Chile

Aram Dorsum: An Extensive Mid‐Noachian Age Fluvial Depositional System in Arabia Terra, Mars

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