Recent Aqueous Environments in Martian Impact Craters: An Astrobiological Perspective

Cabrol, Nathalie A.; Wynn‐Williams, D. D.; Crawford, David A.; Grin, E. A.

doi:10.1006/icar.2001.6661

Cited by 72 publications

(47 citation statements)

References 77 publications

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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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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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“…Moreover, due to the requirement of liquid H 2 O for life as we know it, intra-crater sedimentary deposits have long been suggested as important candidate targets in the search for evidence of past life on Mars (e.g., Grin 1995, 1999;Newsom et al 1996;Grin and Cabrol 1997;Cabrol et al , 2001. Lacustrine sediments are known to provide favorable environments for the preservation of fossils (e.g., slow decay rates; fine sediment grain size; quiet conditions during sedimentation).…”

Section: Introductionmentioning

confidence: 99%

Intra-crater sedimentary deposits at the Haughton impact structure, Devon Island, Canadian High Arctic

Osinski¹,

Lee²

2005

Meteoritics &Amp; Planetary Science

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Abstract-Detailed field mapping has revealed the presence of a series of intra-crater sedimentary deposits within the interior of the Haughton impact structure, Devon Island, Canadian High Arctic. Coarse-grained, well-sorted, pale gray lithic sandstones (reworked impact melt breccias) unconformably overlie pristine impact melt breccias and attest to an episode of erosion, during which time significant quantities of impact melt breccias were removed. The reworked impact melt breccias are, in turn, unconformably overlain by paleolacustrine sediments of the Miocene Haughton Formation. Sediments of the Haughton Formation were clearly derived from pre-impact lower Paleozoic target rocks of the Allen Bay Formation, which form the crater rim in the northern, western, and southern regions of the Haughton structure. Collectively, these field relationships indicate that the Haughton Formation was deposited up to several million years after the formation of the Haughton crater and that they do not, therefore, represent an immediate, post-impact crater lake deposit. This is consistent with new isotopic dating of impactites from Haughton that indicate an Eocene age for the impact event (Sherlock et al. 2005). In addition, isolated deposits of post-Miocene intra-crater glacigenic and fluvioglacial sediments were found lying unconformably over remnants of the Haughton Formation, impact melt breccias, and other pre-impact target rock formations. These deposits provide clear evidence for glaciation at the Haughton crater. The wealth and complexity of geological and climatological information preserved as intra-crater deposits at Haughton suggests that craters on Mars with intra-crater sedimentary records might present us with similar opportunities, but also possibly significant challenges.

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“…Potential sources that may have contributed to aqueous alteration include the early atmosphere; drainage systems, lakes, and other large standing bodies of water (Baker et al, 1991;Newsom et al, 1996;Cabrol et al, 2001;Clifford and Parker, 2001); and the likely presence of shallow and deep aquifers (Clifford, 1993;Forsberg-Taylor et al, 2004).…”

Section: B6 How Was the Chemistry And Mineralogy Of The Early Martiamentioning

confidence: 99%

Key Science Questions from the Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life

et al. 2005

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In October 2004, more than 130 terrestrial and planetary scientists met in Jackson Hole, WY, to discuss early Mars. The first billion years of martian geologic history is of particular interest because it is a period during which the planet was most active, after which a less dynamic period ensued that extends to the present day. The early activity left a fascinating geological record, which we are only beginning to unravel through direct observation and modeling. In considering this time period, questions outnumber answers, and one of the purposes of the meeting was to gather some of the best experts in the field to consider the current state of knowledge, ascertain which questions remain to be addressed, and identify the most promising approaches to addressing those questions. The purpose of this report is to document that discussion. Throughout the planet's first billion years, planetary-scale processes•including differentiation, hydrodynamic escape, volcanism, large impacts, erosion, and sedimentation•rapidly modified the atmosphere and crust. How did these processes operate, and what were their rates and interdependencies? The early environment was also characterized by both abundant liquid water and plentiful sources of energy, two of the most important conditions considered necessary for the origin of life. Where and when did the most habitable environments occur? Did life actually occupy them, and if so, has life persisted on Mars to the present? Our understanding of early Mars is critical to understanding how the planet we see today came to be.

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Recent Aqueous Environments in Martian Impact Craters: An Astrobiological Perspective

Cited by 72 publications

References 77 publications

Episodic flood inundations of the northern plains of Mars

Episodic flood inundations of the northern plains of Mars

Intra-crater sedimentary deposits at the Haughton impact structure, Devon Island, Canadian High Arctic

Key Science Questions from the Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life

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