Sedimentary history and mass flow structures of Chryse and Acidalia Planitiae, Mars

Tanaka, Kenneth L.

doi:10.1029/96je02862

Cited by 173 publications

(177 citation statements)

References 45 publications

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“…(Right) Stratigraphic sequence of Ariadnes inferred from age determinations and spatial relations between units determined in the cartography. At the right, the blue ellipses show the duration of valley networks and the outflow channel activity on Mars (Fassett & Head, 2008;Tanaka, 1997).…”

Section: Geologic Units and Landformsmentioning

confidence: 99%

Geology of the Ariadnes Basin, NE Eridania quadrangle, Mars – 1:1Million

Molina¹,

Pablo²,

Hauber³

et al. 2014

Journal of Maps

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Here we present a 1:1,000,000 geological map of the Ariadnes basin (31 -388 S, 170-1798 E) (Mars), which is one of the topographic depressions located between Terra Sirenum and Terra Cimmeria in the Martian highlands. This basin is diverse, both in terms of morphology and mineralogy, and it is a site of major interest to study the chronological boundary between the Noachian and Hesperian periods ( 3.71 Ga). However, a detailed map of the area has not yet been published. The map described in this paper was produced through the analysis of recent images and topographic data that allow the definition of the geologic units with unprecedented detail. We distinguished eight units and diverse tectonic and geomorphic features. We also examined the regional stratigraphy by age determination using crater counting in order to constrain the geological history of the Ariadnes basin. The map provides a basis for which later analyses can build understanding of the regional paleoenvironment.

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Section: Geologic Units and Landformsmentioning

confidence: 99%

Geology of the Ariadnes Basin, NE Eridania quadrangle, Mars – 1:1Million

Molina¹,

Pablo²,

Hauber³

et al. 2014

Journal of Maps

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“…Overtopping probably did not occur in another circum-Chryse channel because pre-erosion, bowl-shaped craters on the upstream side of some streamlined ]. Although Hampton [1975] noted that as little as 1.5-4% clay mixed into water is sufficient to support even the finest sand and that flows will move on any slope if the debris flow thickness is great enough, and Iida [1938] observed that the extent of mudflows is determined largely by their mobility and is mainly a function of their water content, the long runout of the Chryse channels and mass-flow deposits far into Chryse Planitia [Tanaka, 1997] [Baker, 1979]. Concentrated frazil ice eventually chokes and ponds the flow.…”

mentioning

confidence: 99%

“…Lucchitta [1982b] proposed glacial erosion as a channel-forming process on the basis of some U-shaped valleys in the upper reaches of channels, linear scour marks on the walls of streamlined mounds, grooved terrain similar in scale to that of terrestrial glacial flutes, and the similar dimensions of terrestrial ice rises and streamlined mounds. It also has been suggested that the canyon, chaotic terrains, and channel features are the result of debris flows [Nummedal and Prior, 1981; Jo'ns, 1990; Tanaka, 1997], perhaps generated by local collapse of a hydrologically unstable crust consisting of material of low permeability [MacKinnon and Tanaka, 1989] or by undercooling of water (below equilibrium freezing point) in a basaltic regolith [Gooding, 1987] The image shows a single 75-km-wide, 1-km-deep, channel (black arrow) that almost disappears to resume 100 km downstream (white arrow); where the channel resumes, it is 3 times as wide as above the discontinuity; north toward top, for scale in lower left corner is a120-km-diameter impact crater. channel morphology [Hooke, 1967].…”

mentioning

confidence: 99%

Observations at the Mars Pathfinder site: Do they provide “unequivocal” evidence of catastrophic flooding?

Chapman¹,

Kargel²

1999

J. Geophys. Res.

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Abstract. After Mars Pathfinder landed at the mouth of Ares Vallis, a large channel that drains into the Chryse Planitia basin, the mission reports unanimously supported the interpretation that the lander site is the locus of catastrophic flooding by noting that all aspects of the scene are consistent with this interpretation. However, alternatives cannot be ruled out by any site observations, as all aspects of the scene are equally consistent with other interpretations of origin, namely, ice and mass-flow processes subsequently modified by wind erosion. The authors discuss alternative explanations for the geologic history of the channel based on a regional view of the circum-Chryse channels from Viking images (our best broad-scale information to date) and the local view from the recent Pathfinder landing site. Mega-indicators of channel origin, the regional geomorphology, geology, and planetary climatic conditions, taken together suggest some combination of flood, mass flow, glacial, and eolian processes. The macro-indicators of channel origin (sedimentologic) are also not indicative of one process of emplacement, either as single criteria or taken cumulatively. Finally, the micro-indicators of channel origin (geochemical and mineralogic composition) do not provide very tight constraints on the deposits' possible origins other than that water was in some way involved.

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“…In the first stage, an initial Brown Soil layer was overlain by large rocks which had, or in this stage developed, "Maroon" coatings. These rocks may have been from local volcanic sources, or may have been transported to the site during one of the catastrophic Ares Vallis flood events (e.g., Golombek et al, 1997;Tanaka, 1997). In stage two, smaller, largely uncoated rocks and cobbles were emplaced, possibly as a result of impact events or mechanical weathering of larger, older rocks.…”

Section: Rock Coatingsmentioning

confidence: 99%

“…These channels dissected Noachian-aged southern highlands and Hesperian-aged ridged plains and could have brought materials from these units into the landing ellipse. The floodplain that encompasses the landing site itself was mapped as Hesperian in age (Tanaka et al, 1997). Based on this geologic setting, a diversity of lithologies was expected at the landing site.…”

Section: Introductionmentioning

confidence: 99%

Multispectral imaging from Mars Pathfinder

Farrand¹,

Bell²,

Johnson³

et al. 2008

The Martian Surface

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The Imager for Mars Pathfinder (IMP) was a mast-mounted instrument on the Mars Pathfinder lander which landed on Mars' Ares Vallis floodplain on July 4, 1997. During the 83 sols of Mars Pathfinders landed operations, the IMP collected over 16,600 images. Multispectral images were collected using twelve narrowband filters at wavelengths between 400 and 1000 nm in the visible and near infrared (VNIR) range. The IMP provided VNIR spectra of the materials surrounding the lander including rocks, bright soils, dark soils, and atmospheric observations. During the primary mission, only a single primary rock spectral class, "Gray Rock", was recognized; since then, "Black Rock", has been identified. The Black Rock spectra have a stronger absorption at longer wavelengths than do Gray Rock spectra. A number of coated rocks have also been described, the Red and Maroon Rock classes, and perhaps indurated soils in the form of the Pink Rock class. A number of different soil types were also recognized with the primary ones being Bright Red Drift, Dark Soil, Brown Soil, and Disturbed Soil. Examination of spectral parameter plots indicated two trends which were interpreted as representing alteration products formed in at least two different environmental epochs of the Ares Vallis area. Subsequent analysis of the data and comparison with terrestrial analogs have supported the interpretation that the rock coatings provide evidence of earlier martian environments. However, the presence of relatively uncoated examples of the Gray and Black rock classes indicate that relatively unweathered materials can persist on the martian surface.

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Sedimentary history and mass flow structures of Chryse and Acidalia Planitiae, Mars

Cited by 173 publications

References 45 publications

Geology of the Ariadnes Basin, NE Eridania quadrangle, Mars – 1:1Million

Geology of the Ariadnes Basin, NE Eridania quadrangle, Mars – 1:1Million

Observations at the Mars Pathfinder site: Do they provide “unequivocal” evidence of catastrophic flooding?

Multispectral imaging from Mars Pathfinder

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