Martian impact craters: Correlations of ejecta and interior morphologies with diameter, latitude, and terrain

Barlow, N. G.; Bradley, Tracy L.

doi:10.1016/0019-1035(90)90026-6

Cited by 188 publications

(186 citation statements)

References 25 publications

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“…4. DLE craters are concentrated primarily in topographic lows in the 35-60°N latitude zone, occur in the <3 km to 50 km diameter range, and appear to replace SLE craters within this region (Barlow and Bradley 1990;Barlow and Perez 2003). DLE craters are seen in the corresponding southern hemisphere zone, but in lower concentrations and at higher elevations than those seen in the north (Barlow and Perez 2003;Boyce and MouginisMark 2005).…”

Section: Introductionmentioning

confidence: 98%

“…SLE is the most common ejecta morphology over the entire Martian surface (Mouginis-Mark 1979;Costard 1989;Barlow and Bradley 1990;Barlow and Perez 2003). 2.…”

Section: Introductionmentioning

confidence: 99%

“…2. SLE craters typically range in diameter from ~3 km to 20 km, although they occur over a larger diameter range (both smaller and larger) at high latitudes (MouginisMark 1979;Costard 1989;Barlow and Bradley 1990;Barlow and Perez 2003). 3.…”

Section: Introductionmentioning

confidence: 99%

“…MLE craters are concentrated within the lower to middle latitude regions, particularly along the hemispheric dichotomy boundary. This morphology is primarily associated with craters in the 15 to 60 km diameter range (Barlow and Bradley 1990;Barlow and Perez 2003). These layered morphologies often, but not always, terminate in a distal ridge, and are thus also called rampart craters.…”

Section: Introductionmentioning

confidence: 99%

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Impact craters in the northern hemisphere of Mars: Layered ejecta and central pit characteristics

Barlow

2006

Meteorit & Planetary Scien

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Abstract-Mars Global Surveyor (MGS) and Mars Odyssey data are being used to revise the Catalog of Large Martian Impact Craters. Analysis of data in the revised catalog provides new details on the distribution and morphologic details of 6795 impact craters in the northern hemisphere of Mars. This report focuses on the ejecta morphologies and central pit characteristics of these craters. The results indicate that single-layer ejecta (SLE) morphology is most consistent with impact into an ice-rich target. Double-layer ejecta (DLE) and multiple-layer ejecta (MLE) craters also likely form in volatile-rich materials, but the interaction of the ejecta curtain and target-produced vapor with the thin Martian atmosphere may be responsible for the large runout distances of these ejecta. Pancake craters appear to be a modified form of double-layer craters where the thin outer layer has been destroyed or is unobservable at present resolutions. Pedestal craters are proposed to form in an icerich mantle deposited during high obliquity periods from which the ice has subsequently sublimated. Central pits likely form by the release of vapor produced by impact into ice-soil mixed targets. Therefore, results from the present study are consistent with target volatiles playing a dominant role in the formation of crater morphologies found in the Martian northern hemisphere.

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Section: Introductionmentioning

confidence: 98%

“…SLE is the most common ejecta morphology over the entire Martian surface (Mouginis-Mark 1979;Costard 1989;Barlow and Bradley 1990;Barlow and Perez 2003). 2.…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Impact craters in the northern hemisphere of Mars: Layered ejecta and central pit characteristics

Barlow

2006

Meteorit & Planetary Scien

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“…Long-term aqueous activity on the surface of the planet is indicated by fluvial (e.g., Mars Channel Working Group, 1983;Edgett, 2000a, 2000b) and lacustrine features (e.g., Squyres, 1989;Grin, 1999, 2001); phased degradation of impact craters (e.g., Chapman and Jones, 1977;Craddock and Maxwell, 1993); permafrost (e.g., Lucchitta, 1981); periglacial (e.g., Squyres, 1979) and glacial landforms (e.g., Lucchitta, 1982;Kargel et al, 1995); and outflow channels (e.g., Baker and outflow channels, which either terminate at the boundary (Parker et al, 1993) or fade into the northern plains (Ivanov and Head, 2001), including the prominent circum-Chryse (e.g., Rotto and Tanaka, 1995) and recently identified northwestern slope valleys (NSVs, Dohm et al, 2000Dohm et al, , 2001a outflow channel systems; (3) the relatively low density of superposed impact craters in the northern plains compared to the southern densely cratered highlands (Barlow and Bradley, 1990;Parker et al, 1993), and its extremely flat topography at the distal reaches of the outflow channel systems (Head et al, 1999); (4) the broad occurrence of wide age-ranging glaciers that are interpreted to be linked to magmatic-triggered flooding and associated short-lived (tens of thousands of years) environmental/climatic changes (Baker, 2001;Cabrol et al, 2001aCabrol et al, , 2001bCabrol et al, , 2001c; and (5) the chemical signatures reported for the northern plains, including high abundances of S and Cl or the possible existence of sulphate minerals and chloride salts, making a putative andesite-rich component or weathered basalt the dominant material type in the lowlands (McSween et al, 1999;Zuber, 2001;Wyatt and McSween, 2002). Standing bodies of water, therefore, best explain such evidence, though volcanism , tectonism (Sleep, 1994), eolian modification (Malin and Edgett, 2000a), ground volatile and debris flow activity along the highland-lowland boundary (Tanaka, 1997;…”

Section: Introductionmentioning

confidence: 99%

Episodic flood inundations of the northern plains of Mars

Fairén

Dohm

Baker

et al. 2003

Icarus

168

160

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Throughout the recorded history of Mars, liquid water has distinctly shaped its landscape, including the prominent circum-Chryse and the northwestern slope valleys outflow channel systems, and the extremely flat northern plains topography at the distal reaches of these outflow channel systems. Paleotopographic reconstructions of the Tharsis magmatic complex reveal the existence of an Europe-sized Noachian drainage basin and subsequent aquifer system in eastern Tharsis. This basin is proposed to have sourced outburst floodwaters that sculpted the outflow channels, and ponded to form various hypothesized oceans, seas, and lakes episodically through time. These floodwaters decreased in volume with time due to inadequate groundwater recharge of the Tharsis aquifer system. Martian topography, as observed from the Mars Orbiter Laser Altimeter, corresponds well to these ancient flood inundations, including the approximated shorelines that have been proposed for the northern plains. Stratigraphy, geomorphology, and topography record at least one great Noachian-Early Hesperian northern plains ocean, a Late Hesperian sea inset within the margin of the high water marks of the previous ocean, and a number of widely distributed minor lakes that may represent a reduced Late Hesperian sea, or ponded waters in the deepest reaches of the northern plains related to minor Tharsis-and Elysium-induced Amazonian flooding.

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Fresh shallow valleys in the Martian midlatitudes as features formed by meltwater flow beneath ice

2014

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Significant numbers of valleys have been identified in the Martian midlatitudes (30-60°N/S), spatially associated with extant or recent ice accumulations. Many of these valleys date to the Amazonian, but their formation during these cold, dry epochs is problematic. In this study, we look in detail at the form, distribution, and quantitative geomorphology of two suites of these valleys and their associated landforms in order to better constrain the processes of their formation. Since the valleys themselves are so young and thus well preserved, uniquely, we can constrain valley widths and courses and link these to the topography from the Mars Orbiter Laser Altimeter and High-Resolution Stereo Camera data. We show that the valleys are both qualitatively and quantitatively very similar, despite their being >5000 km apart in different hemispheres and around 7 km apart in elevation. Buffered crater counting indicates that the ages of these networks are statistically identical, probably forming during the Late Amazonian,~100 Ma. In both localities, at least tens of valleys cross local drainage divides, apparently flowing uphill. We interpret these uphill reaches to be characteristic of flow occurring beneath a now absent, relatively thin (order 10 1 -10 2 m), regionally extensive ice cover. Ridges and mounds occasionally found at the foot of these valley systems are analogous to eskers and aufeis-like refreezing features. On the basis of their interaction with these aufeis-like mounds, we suggest that this suite of landforms may have formed in a single, short episode (perhaps order of days), probably forced by global climate change.

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Martian impact craters: Correlations of ejecta and interior morphologies with diameter, latitude, and terrain

Cited by 188 publications

References 25 publications

Impact craters in the northern hemisphere of Mars: Layered ejecta and central pit characteristics

Impact craters in the northern hemisphere of Mars: Layered ejecta and central pit characteristics

Episodic flood inundations of the northern plains of Mars

Fresh shallow valleys in the Martian midlatitudes as features formed by meltwater flow beneath ice

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