Amazonian geologic history of the Echus Chasma and Kasei Valles system on Mars: New data and interpretations

Chapman, M. G.; Neukum, G.; Dumke, A.; Michael, Greg; Gasselt, S. van; Kneissl, T.; Zuschneid, W.; Hauber, Ernst; Mangold, N.

doi:10.1016/j.epsl.2009.11.034

Cited by 79 publications

(28 citation statements)

References 30 publications

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“…A glacial mantle deposit could also explain why some North of Echus Chasma the radar-bright terrain traces where the At 5 flows extend as a peninsula (284°E, 16°N) into the radardark head-region of Kasei Valles. In this region, and farther north and west, the radar features conform more closely to the recent geologic map of Chapman et al (2010) than to the older map of Scott and Tanaka (1986). The Chapman et al map shows the At 5 flows extending up to 20°N latitude, where they share a boundary with the older (Hesperian) Ht 4 flows.…”

Section: East Tharsis Flows and Minor Shieldsmentioning

confidence: 88%

“…This agrees with the geologic map of Scott and Tanaka (1986), which has the At 5 flows extending south and embaying most of this leg-shaped chasma. A more recent study (Chapman et al, 2010) suggests a more complex volcanic sequence for Echus Chasma, in which older ''platy-ridged'' flows (their unit Apf), possibly originating in the chasma itself, are overlain or embayed by younger At 5 flows. Platy-ridged flows have also been identified in the chasma by Mangold et al (2010).…”

Section: East Tharsis Flows and Minor Shieldsmentioning

confidence: 99%

“…These flows are similar to radar-bright platy flows seen in Cerberus and Marte Vallis (Section 5.3) and southern Amazonis (Section 6.2). Chapman et al (2010) mapped Apf outcrops in the ankle, foot, and lower calf of Echus, and portions of these are among the radar-brightest regions of the chasma. These authors suggest that the ''foot'' region is covered by a thin lacustrine material (unit Apec) similar to the sedimentary deposit (unit Avf) mapped in this same region by Scott and Tanaka (1986).…”

Section: East Tharsis Flows and Minor Shieldsmentioning

confidence: 99%

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Arecibo radar imagery of Mars: The major volcanic provinces

Harmon¹,

Nolan²,

Husmann³

et al. 2012

Icarus

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Section: East Tharsis Flows and Minor Shieldsmentioning

confidence: 88%

Section: East Tharsis Flows and Minor Shieldsmentioning

confidence: 99%

Section: East Tharsis Flows and Minor Shieldsmentioning

confidence: 99%

See 1 more Smart Citation

Arecibo radar imagery of Mars: The major volcanic provinces

Harmon¹,

Nolan²,

Husmann³

et al. 2012

Icarus

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“…A cycle lasting from 1.8-1.0 Ga began with fluvial erosion of a narrow channel in the Tharsis Montes formation in north Kasei Valles followed by episodic catastrophic floods sourced from Echus Chasma. A massive 2100-km-runout of flood lavas from Echus Chasma occurred between 205 and 128 Ma (Chapman et al, 2010b).…”

Section: Geologic Histories and Mappingmentioning

confidence: 99%

“…(1) The large areal extent of single HRSC nadir images (minimum width of 62.5 km at 12.5 m/pixel and variable lengths up to several 1000 km) are particularly favorable for mapping of volcanic deposits and edifices at scales of about 1:40,000 (e.g., Bleacher et al, 2007aBleacher et al, , 2007bChapman et al, 2010aChapman et al, , 2010bPlatz and Michael, 2011;Hauber, 2012, 2013). Colored views of the Martian surface based on the red, green, blue, and near-infrared channels also deliver additional information that assist in distinguishing surface domains, and when combined with OMEGA data in particular and provide information on the composition of volcanic materials.…”

Section: Endogenic Processesmentioning

confidence: 99%

Quantifying geological processes on Mars—Results of the high resolution stereo camera (HRSC) on Mars express

Jaumann

Tirsch

Hauber

et al. 2015

Planetary and Space Science

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a b s t r a c tThis review summarizes the use of High Resolution Stereo Camera (HRSC) data as an instrumental tool and its application in the analysis of geological processes and landforms on Mars during the last 10 years of operation. High-resolution digital elevations models on a local to regional scale are the unique strength of the HRSC instrument. The analysis of these data products enabled quantifying geological processes such as effusion rates of lava flows, tectonic deformation, discharge of water in channels, formation timescales of deltas, geometry of sedimentary deposits as well as estimating the age of geological units by crater size-frequency distribution measurements. Both the quantification of geological processes and the age determination allow constraining the evolution of Martian geologic activity in space and time. A second major contribution of HRSC is the discovery of episodicity in the intensity of geological processes on Mars. This has been revealed by comparative age dating of volcanic, fluvial, glacial, and lacustrine deposits.Volcanic processes on Mars have been active over more than 4 Gyr, with peak phases in all three geologic epochs, generally ceasing towards the Amazonian. Fluvial and lacustrine activity phases spread a time span from Noachian until Amazonian times, but detailed studies show that they have been interrupted by multiple and long Contents lists available at ScienceDirect

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Hydrological and sedimentary analyses of well-preserved paleofluvial-paleolacustrine systems at Moa Valles, Mars

Salese

Achille

Neesemann

et al. 2016

J. Geophys. Res. Planets

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Moa Valles is a well‐preserved, likely Amazonian (younger than 2 Ga old), paleodrainage system that is nearly 300 km long and carved into ancient highland terrains west of Idaeus Fossae. The fluvial system apparently originated from fluidized ejecta blankets, and it consists of a series of dam breach paleolakes with associated fan‐shaped sedimentary deposits. The paleolakes are interconnected and drain eastward into Liberta crater, forming a complex and multilobate deltaic deposit exhibiting a well‐developed channelized distributary pattern with evidence of switching on the delta plain. A breach area, consisting of three spillover channels, is present in the eastern part of the crater rim. These channels connect the Liberta crater to the eastward portion of the valley system, continuing toward Moa Valles with a complex pattern of anabranching channels that is more than 180 km long. Based on hydrological calculations of infilling and spillover discharges of the Liberta crater lake, the formation of the whole fluvial system is compatible with short to medium (<1000 year) timescales, although the length and morphology of the observed fluvial‐lacustrine features suggest long‐term periods of activity based on terrestrial analogs. Water for the 300 km long fluvial system may have been primarily sourced by the melting of shallow ice due to the thermal anomaly produced by impact craters. The occurrence of relatively recent (likely Amazonian) hydrological activity, which could have been primarily supported by groundwater replenishment, supports the hypothesis that hydrological activity could have been possible after the Noachian‐Hesperian boundary, which is commonly considered as the onset epoch of the present cold‐dry climate.

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Amazonian geologic history of the Echus Chasma and Kasei Valles system on Mars: New data and interpretations

Cited by 79 publications

References 30 publications

Arecibo radar imagery of Mars: The major volcanic provinces

Arecibo radar imagery of Mars: The major volcanic provinces

Quantifying geological processes on Mars—Results of the high resolution stereo camera (HRSC) on Mars express

Hydrological and sedimentary analyses of well-preserved paleofluvial-paleolacustrine systems at Moa Valles, Mars

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