Geology of the Reull Vallis Region, Mars

Mest, S. C.; Crown, D. A.

doi:10.1006/icar.2001.6655

Cited by 56 publications

(90 citation statements)

References 46 publications

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“…Photogeologic mapping at 1:500,000 scale from analysis of Viking Orbiter images complements volcanological studies of Hadriaca Patera, geologic investigations of the other highland paterae, and an analysis of the styles and evolution of volcanic activity east of Hellas Planitia in the ancient, cratered highlands of Mars (Greeley and Crown, 1990;Crown and Greeley, 1993). This photogeologic study is an extension of regional geologic mapping east of Hellas Planitia (Crown and others, 1992;Mest and Crown, 2001).…”

Section: Introductionmentioning

confidence: 66%

“…The area east of Hellas Planitia is a complex geologic region affected by volcanism, tectonism, and channel-and canyon-forming processes (Crown and others, 1992;Tanaka and Leonard, 1995;Gregg and others, 1998;Price, 1998;Leonard and Tanaka, 2001;Mest and Crown, 2001;Crown and others, 2005b). The Hadriaca Patera summit region is dominated by the central caldera and eroded flanks of the volcano.…”

Section: General Geologymentioning

confidence: 99%

“…From an energy perspective, both magmatic and hydromagmatic eruption models are viable (Crown and Greeley, 1993). Geomorphic analyses and mapping indicate an extended and complex history of volatile-driven activity in the region surrounding Hadriaca Patera (Crown and others, 1992;Mest and Crown, 2001;Crown and others, 2005b). The regional geologic setting and analyses of the potential supply of groundwater are consistent with hydrovolcanic activity (Crown and Greeley, 1993).…”

Section: Stratigraphymentioning

confidence: 99%

“…Peraea Cavus and Ausonia Cavus are separated from the main canyons of Dao and Niger Valles (south of map area) by zones of collapsed and subsided plains (Squyres and others, 1987;Crown and others, 1992;Mest and Crown, 2001;Crown and others, 2004). These materials are mapped as irregular vallis floor material (unit AHvi), which exhibits surfaces dissected by small channels and troughs.…”

Section: Stratigraphymentioning

confidence: 99%

See 3 more Smart Citations

Geologic Map of the MTM -30262 and -30267 Quadrangles, Hadriaca Patera Region of Mars

Crown¹,

Greeley²

2007

Scientific Investigations Map

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Section: Introductionmentioning

confidence: 66%

Section: General Geologymentioning

confidence: 99%

Section: Stratigraphymentioning

confidence: 99%

Section: Stratigraphymentioning

confidence: 99%

See 2 more Smart Citations

Geologic Map of the MTM -30262 and -30267 Quadrangles, Hadriaca Patera Region of Mars

Crown¹,

Greeley²

2007

Scientific Investigations Map

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“…Nature, however, is always more complicated than simple models, and the subsurface materials of Noachian and Hesperian uplands, though weak, may involve complex layering. Tanaka et al (1988), Crown et al (1992), Mest and Crown (2001), and many others have documented from stratigraphic and morphologic considerations that ancient fluvial, periglacial, volcanic eolian materials are probably interbedded among the putative weakly cemented impact ejecta layers in the old uplands. Carbonate-cemented layers in southwestern U.S. deserts, for example, can be quite strong but are commonly found in thin layers interbedded with crumbly alluvium.…”

Section: Regolith Production and Its Effect On Materials Propertiesmentioning

confidence: 99%

Nature of the Martian uplands: Effect on Martian meteorite age distribution and secondary cratering

Hartmann

Barlow

2006

Meteorit & Planetary Scien

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Abstract-Martian meteorites (MMs) have been launched from an estimated 5-9 sites on Mars within the last 20 Myr. Some 80-89% of these launch sites sampled igneous rock formations from only the last 29% of Martian time. We hypothesize that this imbalance arises not merely from poor statistics, but because the launch processes are dominated by two main phenomena: first, much of the older Martian surface is inefficient in launching rocks during impacts, and second, the volumetrically enormous reservoir of original cumulate crust enhances launch probability for 4.5 Gyr old rocks.There are four lines of evidence for the first point, not all of equal strength. First, impact theory implies that MM launch is favored by surface exposures of near-surface coherent rock (≤10 2 m deep), whereas Noachian surfaces generally should have ≥10 2 m of loose or weakly cemented regolith with high ice content, reducing efficiency of rock launch. Second, similarly, both Mars Exploration Rovers found sedimentary strata, 1-2 orders of magnitude weaker than Martian igneous rocks, favoring low launch efficiency among some fluvial-derived Hesperian and Noachian rocks. Even if launched, such rocks may be unrecognized as meteorites on Earth. Third, statistics of MM formation age versus cosmic-ray exposure (CRE) age weakly suggest that older surfaces may need larger, deeper craters to launch rocks. Fourth, in direct confirmation, one of us (N. G. B.) has found that older surfaces need larger craters to produce secondary impact crater fields (cf. Barlow and Block 2004). In a survey of 200 craters, the smallest Noachian, Hesperian, and Amazonian craters with prominent fields of secondaries have diameters of ~45 km, ~19 km, and ~10 km, respectively. Because 40% of Mars is Noachian, and 74% is either Noachian or Hesperian, the subsurface geologic characteristics of the older areas probably affect statistics of recognized MMs and production rates of secondary crater populations, and the MM and secondary crater statistics may give us clues to those properties.

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Constraints on the formation and properties of a Martian lobate debris apron: Insights from high‐resolution topography, SHARAD radar data, and a numerical ice flow model

Parsons

Holt

2016

JGR Planets

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Lobate debris aprons (LDAs) are midlatitude deposits of debris‐covered ice formed during one or more periods of glaciation during the Amazonian period. However, little is known about the climate conditions that led to LDA formation. We explore a hypothesis in which a single, extended period of precipitation of ice on the steep slopes of Euripus Mons (45°S, 105°E—east of the Hellas Basin) produced a flowing ice deposit which was protected from subsequent ablation to produce the LDA found at this location. We test this hypothesis with a numerical ice flow model using an ice rheology based on low‐temperature ice deformation experiments. The model simulates ice accumulation and flow for the northern and southern lobes of the Euripus Mons LDA using basal topography constrained by data from the Shallow Radar (SHARAD) and a range of ice viscosities (determined by ice temperature and ice grain size). Simulations for the northern lobe of the Euripus LDA produce good fits to the surface topography. Assuming an LDA age of ∼60 Myr and an expected temperature range of 200 to 204 K (for various obliquities) gives an ice grain size of ≈2 mm. Simulations of the southern section produce poor fits to surface topography and result in much faster flow timescales unless multiple ice deposition events or higher ice viscosities are considered.

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Geology of the Reull Vallis Region, Mars

Cited by 56 publications

References 46 publications

Geologic Map of the MTM -30262 and -30267 Quadrangles, Hadriaca Patera Region of Mars

Geologic Map of the MTM -30262 and -30267 Quadrangles, Hadriaca Patera Region of Mars

Nature of the Martian uplands: Effect on Martian meteorite age distribution and secondary cratering

Constraints on the formation and properties of a Martian lobate debris apron: Insights from high‐resolution topography, SHARAD radar data, and a numerical ice flow model

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