Hypotheses for the origin of the Hypanis fan-shaped deposit at the edge of the Chryse escarpment, Mars: Is it a delta?

Adler, John H.; Bell, James F.; Fawdon, P.; Davis, J. M.; Warner, N. H.; Sefton‐Nash, E.; Harrison, Tanya N.

doi:10.1016/j.icarus.2018.05.021

Cited by 30 publications

(50 citation statements)

References 65 publications

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“…In either case, the presence of sand is second cause for the lower thermal contrast here. In another example, at the distal end of Hypanis Valles (e.g., Adler et al, ; Fawdon et al, ), FSRs have lower thermal inertia than surrounding plains due to the breakdown of deposits (Figure 10). HiRISE images show eolian ripples confined to the inverted fluvial landform.…”

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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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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“…(Deltas existed at Eberswalde and Holden, and evidence has been reported for deltas at many other sites -e.g. Lewis & Aharonson 2006, Grant et al 2008, Metz et al 2009b, di Achille & Hynek 2010, Goudge et al 2017, Adler et al 2019. Multiplying delta volume by assumed water:sediment volume ratio >10 2 gives (at Eberswalde, SW Melas, and Gale) a cumulative water volume that is far in excess of the paleo-lake volume.…”

Section: τ: Duration Of Longest Individual River-forming Climate: >(1mentioning

confidence: 99%

Geologic Constraints on Early Mars Climate

Kite

2019

Space Sci Rev

109

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Early Mars climate research has well-defined goals (Mars Exploration Program Analysis Group 2018). Achieving these goals requires geologists and climate modelers to coordinate. Coordination is easier if results are expressed in terms of well-defined parameters. Key parameters include the following quantitative geologic constraints.(1) Cumulative post-3.4 Ga precipitation-sourced water runoff in some places exceeded 1 km column. (2) There is no single Early Mars climate problem: the traces of ≥2 riverforming periods are seen. Relative to rivers that formed earlier in Mars history, rivers that formed later in Mars history are found preferentially at lower elevations, and show a stronger dependence on latitude. (3) The duration of the longest individual river-forming climate was >(10 2 -10 3 ) yr, based on paleolake hydrology. (4) Peak runoff production was >0.1 mm/hr. However, (5) peak runoff production was intermittent, sustained (in a given catchment) for only <10% of the duration of river-forming climates. (6) The cumulative number of wet years during the valley-network-forming period was >10 5 yr. (7) Post-Noachian light-toned, layered sedimentary rocks took >10 7 yr to accumulate. However, (8) an "average" place on Mars saw water for <10 7 yr after the Noachian, suggesting that the river-forming climates were interspersed with long globally-dry intervals. (9) Geologic proxies for Early Mars atmospheric pressure indicate pressure was not less than 0.012 bar but not much more than 1 bar. A truth table of these geologic constraints versus currently published climate models shows that the late persistence of river-forming climates, combined with the long duration of individual lake-forming climates, is a challenge for most models. Kraal, Erin R.; Asphaug, Erik; Moore, Jeffery M.; Howard, Alan; Bredt, Adam, 2008a, Catalogue of large alluvial fans in martian impact craters, Icarus, 194, 1, 101-110. Kraal, Erin R.; van Dijk, Maurits; Postma, George; Kleinhans, Maarten G., 2008b, Martian stepped-delta formation by rapid water release, Nature, 451, 7181, 973-976.Kurahashi-Nakamura, Takasumi; Tajika, Eiichi, 2006, Atmospheric collapse and transport of carbon dioxide into the subsurface on early Mars, Geophys. Res. Lett., 33, L18205.

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“…DEMs enable an understanding of 3-D form and process relationships otherwise only available through in situ study. These include investigations of recurring slope lineations (Schaefer et al, 2019), glacial deposits (Hubbard et al, 2011;Conway and Balme, 2014), aeolian ridges (Berman et al, 2018;Chojnacki et al, 2014Chojnacki et al, , 2017, and fluvial deposits (Voigt and Hamilton, 2018;Tirsch et al, 2018;Adler et al, 2019;Davis et al, 2018;Hamilton et al, 2018;Stack et al, 2016;Wilson et al, 2018). DEMs also fulfil a critical mission requirement when searching for potential rover landing sites (Stack et al, 2016;Golombek et al, 2017Golombek et al, , 2012Grant et al, 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Notably, our methods presented herein are focussed on the proof of concept and functionality of this new pipeline. The AU pipeline is designed to be rapidly and freely implemented by researchers and is based on the open-source suite of automated geodesy and stereogrammetry tools from the NASA intelligent systems division called the Ames Stereo Pipeline (ASP) (Moratto et al, 2010;Beyer et al, 2018) and the Integrated Software for Imagers and Spectrometers version 3.5.3 programme (ISIS v3.5.3) (Anderson et al, 2004;Anderson, 2008). Several pipelines already exist for the generation of HiRISE and CTX digital elevation models, using both open-source and commercial software.…”

Section: Introductionmentioning

confidence: 99%

Creating HiRISE digital elevation models for Mars using the open-source Ames Stereo Pipeline

Hepburn

Holt

Hubbard

et al. 2019

Geosci. Instrum. Method. Data Syst.

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Abstract. The present availability of sub-decametre digital elevation models on Mars – crucial for the study of surface processes – is scarce. In contrast to low-resolution global datasets, such models enable the study of landforms <10 km in size, which is the primary scale at which geomorphic processes have been active on Mars over the last 10–20 Myr . Stereogrammetry is a means of producing digital elevation models from stereo pairs of images. The HiRISE camera on board the Mars Reconnaissance Orbiter has captured >3000 stereo pairs at 0.25 m pixel−1 resolution, enabling the creation of high-resolution digital elevation models (1–2 m pixel−1). Hitherto, only ∼500 of these pairs have been processed and made publicly available. Existing pipelines for the production of digital elevation models from stereo pairs, however, are built upon commercial software, rely upon sparsely available intermediate data, or are reliant on proprietary algorithms. In this paper, we present and test the output of a new pipeline for producing digital elevation models from HiRISE stereo pairs that is built entirely upon the open-source NASA Ames Stereo Pipeline photogrammetric software, making use of freely available data for cartographic rectification. This pipeline is designed for simple application by researchers interested in the use of high-resolution digital elevation models. Implemented here on a research computing cluster, this pipeline can also be used on consumer-grade UNIX computers. We produce and evaluate four digital elevation models using the pipeline presented here. Each are globally well registered, with accuracy similar to those of digital elevation models produced elsewhere.

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Hypotheses for the origin of the Hypanis fan-shaped deposit at the edge of the Chryse escarpment, Mars: Is it a delta?

Cited by 30 publications

References 65 publications

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

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

Geologic Constraints on Early Mars Climate

Creating HiRISE digital elevation models for Mars using the open-source Ames Stereo Pipeline

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