Geology of Aeolis Dorsa alluvial sedimentary basin, Mars

Pietro, Ilaria Di; Ori, G. G.; Pondrelli, M.; Salese, F.

doi:10.1080/17445647.2018.1454350

Cited by 58 publications

(15 citation statements)

References 22 publications

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“…Davis et al (2019Davis et al ( , 2016 presented evidence for an extensive network of Noachian age depositional fluvial channel belts, now exposed in inverted relief, within erosional windows in the Arabia Terra region. These fluvial systems, and others previously described in the Aeolis Dorsa region (e.g., Burr et al, 2010;Cardenas et al, 2018;Di Pietro et al, 2018;DiBiase et al, 2013;Hughes et al, 2019;Kite et al, 2015;, are consistent with formation by self-formed channels in an aggradational alluvial environment (Davis et al, 2019(Davis et al, , 2016. Although many of the sinuous ridges that define these inverted channels are discontinuous and heavily eroded, a few examples are well preserved and have sufficient exposure for detailed analysis with orbital remote sensing data.…”

Section: Introductionsupporting

confidence: 85%

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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Section: Introductionsupporting

confidence: 85%

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

et al. 2020

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“…After reviewing thermophysical characteristics of Martian FSRs from a global database (Williams, ), 20 locations were selected for this study that are representative of the geographic distribution of these landforms (Figure 1). FSRs are concentrated in Arabia Terra (Davis et al, ) and the Aeolis/Zephyria Plana (AZP) region (Burr et al, , ; Di Pietro et al, ; DiBiase et al, ). Scattered examples are located in the Valles Marineris canyon system (e.g., Weitz et al, ), Margaritifer Terra, Solis Dorsa, and the circum‐Chryse basin.…”

Section: Resultsmentioning

confidence: 99%

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

Williams

Moersch

Fergason

2018

Earth and Space Science

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In denuded landscapes, terrestrial inverted fluvial landforms are preferentially preserved due to their greater resistance to erosion from clast armoring, lava infilling, or cementation. These induration agents have differing material properties that should influence the thermal response of the surface. Using thermal inertia derived from 2001 Mars Odyssey Thermal Emission Imaging System (THEMIS) data, we find that the thermophysical contrast for 20 large "inverted channels" on Mars is comparable or elevated in comparison to nearby well-indurated materials. The fluvial sinuous ridge (FSR) thermal signature, together with regional geology and morphology attributes, leads us to disfavor clast armoring as an induration agent for most Martian FSRs. The available evidence is consistent with cementation as the most likely induration agent for FSRs, although lava infilling is a plausible explanation especially for instances of nearby volcanic edifices. FSR cementation, probably by near-surface solute-rich groundwater, extends aqueous processes beyond the period of widespread fluvial activity. Future work on the temporal response of the surfaces of inverted channels has the potential to further test the inferred induration mechanism and potentially constrain the grain size distribution.

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“…Martian inverted channels are identified as extensive networks across intercrater plains ( Burr et al, 2010 ; Davis et al, 2016 ; Di Pietro et al, 2018 ), on crater floor plains ( Irwin III et al, 2018 ), and in association with multiple proposed and selected rover landing sites (e.g., Anderson and Bell, 2010 ; Irwin III et al, 2015 ; Palucis et al, 2014 ; Balme et al, 2020 ) including the Perseverance field site at Jezero crater ( Goudge et al, 2018 ). The interpretation of Martian ridges as relict fluvial landforms is strengthened at sites with strong geologic context (e.g., Davis et al, 2019 ), but there are many locations where the origin of ridges is ambiguous or could be explained by alternate hypotheses such as structural features, dikes or eskers (e.g., Banks et al, 2009 ; Butcher et al, 2021 ).…”

Section: Discussionmentioning

confidence: 99%

“…On this point, we discuss several specific inverted channel attributes: Planform . There is a natural tendency to connect ridge segments in planetary mapping using orbital images (e.g., Di Pietro et al, 2018 ). However, considering the landscape as a ‘snapshot’ and linking inverted channel segments to define the former interconnected network may result in an inaccurate view of the depositional history.…”

Section: Discussionmentioning

confidence: 99%

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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Geology of Aeolis Dorsa alluvial sedimentary basin, Mars

Cited by 58 publications

References 22 publications

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

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

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

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

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