Origin and evolution of the layered deposits in the Valles Marineris, Mars

Nedell, Susan S.; Squyres, S. W.; Andersen, David W.

doi:10.1016/0019-1035(87)90086-8

Cited by 182 publications

(144 citation statements)

References 23 publications

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“…Additionally, the recent apparent evidence for the role of water in the formation of hematite and its associated deposits at the Meridiani landing site (e.g., Christensen et al 2004;Herkenhoff et al 2004) seems to discount the possibility that the Meridiani hematite represents a hematite coating produced during extrusion of a glassy basalt flow. Given similar, water-related sedimentary origins proposed for the hematite-associated materials in Aram Chaos and Valles Marineris (Nedell et al 1987;Christensen et al 2001b;Glotch and Christensen 2003;Weitz et al 2003), it may also be unlikely that hematite-coated basalts like those in this study are the source of the hematite signature in these regions. However, formation of the gray hematite in Aram Chaos and Valles Marineris by glassy basalt flow oxidation during extrusion should not be discounted as these sites are studied further.…”

Section: Discussionmentioning

confidence: 99%

A new hematite formation mechanism for Mars

Minitti

Lane

Bishop

2005

Meteorit & Planetary Scien

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Abstract-The origin of hematite detected in Martian surface materials is commonly attributed to weathering processes or aqueous precipitation. Here, we present a new hematite formation mechanism that requires neither water nor weathering. Glass-rich basalts with Martian meteorite-like chemistry (high FeO, low Al 2 O 3 ) oxidized at high (700 and 900 °C) temperatures in air and CO 2 , respectively, form thin (<1 µm) hematite coatings on their outermost surfaces. Hematite is manifested macroscopically by development of magnetism and a gray, metallic sheen on the glass surface and microscopically by Fe enrichment at the glass surface observed in element maps. Visible and nearinfrared, thermal infrared, and Raman spectroscopy confirm that the Fe enrichment at the oxidized glass surfaces corresponds to hematite mineralization. Hematite formation on basaltic glass is enabled by a mechanism that induces migration of Fe 2+ to the surface of an oxidizing glass and subsequent oxidation to form hematite. A natural example of the hematite formation mechanism is provided by a Hawaiian basalt hosting a gray, metallic sheen that corresponds to a thin hematite coating. Hematite coating development on the Hawaiian basalt demonstrates that Martian meteorite-like FeO contents are not required for hematite coating formation on basalt glass and that such coatings form during initial extrusion of the glassy basalt flows. If gray hematite originating as coatings on glassy basalt flows is an important source of Martian hematite, which is feasible given the predominance of igneous features on Mars, then the requirement of water as an agent of hematite formation is eliminated.

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Section: Discussionmentioning

confidence: 99%

A new hematite formation mechanism for Mars

Minitti

Lane

Bishop

2005

Meteorit & Planetary Scien

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“…Many theories for their formation have been put forward, including subaerial 58 fluvial deposition or volcanism (Lucchitta et al, 1992), accumulation of eolian dust or sand 59 (Peterson, 1981), evaporite precipitation in lakes (McKay and Nedell, 1988) or from 60 groundwater (Murchie et al, 2009a), subaqueous (Nedell et al, 1987) or sub-ice volcanism 61 (Chapman and Tanaka, 2001), or the formation as spring deposits (Rossi et al, 2008), but a 62 conclusive theory combining all implications suggested by the composition, structure and 63 stratigraphic position of these deposits is still missing. A detailed discussion of the shortcomings 64 of each of the formation theories is provided by Lucchitta, 2009a;2009b.…”

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confidence: 99%

Sulfates and iron oxides in Ophir Chasma, Mars, based on OMEGA and CRISM observations

Wendt

Gross

Kneissl

et al. 2011

Icarus

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“…Nevertheless, landing inside Valles Marineris would provide spectacular views of adjacent canyon walls and likely access to enigmatic layered deposits (McCauley, 1978). These layered deposits have been interpreted as mass wasting, carbonate, eolian, and volcanic deposits (e.g., McCauley, 1978;Nedell et al, 1987;Lucchitta, 1989;Malin and Edgett, 2000;Chapman and Tanaka, 2001). Understanding their origin may shed new light on the evolution of the Valles Marineris system.…”

Section: Overview Of the Top Sitesmentioning

confidence: 99%