The nature of coarse-grained crystalline hematite and its implications for the early environment of Mars

Catling, David C.; Moore, Jeffrey M.

doi:10.1016/s0019-1035(03)00173-8

Cited by 147 publications

(143 citation statements)

References 111 publications

Supporting

Mentioning

141

Contrasting

Order By: Relevance

“…ILDs in Iani Chaos show layering on multiple scales (Bridges et al, 2008;Warner et al, 2011), exhibit higher thermal inertias than surrounding terrains (Glotch and Rogers, 2007) and are sometimes topped by dark 'cap' units, similar to those in Juventae Chasma (Catling et al, 2006), Aram Chaos (Catling and Moore, 2003;Glotch and Rogers, 2007), Mawrth Vallis (Loizeau et al, 2010) and Valles Marineris (Komatsu et al, 2004). ILDs are almost always associated with detections of sulphate minerals, which are often hydrated (Bibring et al, 2006;Bishop et al, 2009;Gendrin et al, 2005), and some are reported to show spectral features indicative of phyllosilicates (Grindrod et al, 2012;Weitz et al, 2011).…”

Section: Ilds In Iani Chaosmentioning

confidence: 99%

Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars

Sefton‐Nash

Catling

Wood

et al. 2012

Icarus

View full text Add to dashboard Cite

a b s t r a c tWe present an analysis of Interior Layered Deposits (ILDs) in Iani Chaos using visible, infrared, hyperspectral and topographic datasets acquired by instruments aboard NASA's Mars Global Surveyor, Mars Odyssey, Mars Reconnaissance Orbiter and ESA's Mars Express spacecraft. We focus on four main regions where ILDs outcrop in Iani Chaos. Deposits span a $2 km range of elevations and exhibit moderate to high albedos, layering at sub-decameter scales, thermal inertias of 300-800 J m À2 K À1 s À1/2 and a range of surface textures. Thermal inertia calculations use slope and azimuth corrections from High Resolution Stereo Camera (HRSC) topography. Spectral features in hyperspectral data acquired by NASA's Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) suggest that gypsum (CaSO 4 Á2H 2 O) and kieserite (MgSO 4 ÁH 2 O) are present in most deposits. We report absorptions typically exhibited by alunite (KAl 3 (SO 4 ) 2 (OH) 6 ) and jarosite KFe 3þ 3 ðOHÞ 6 ðSO 4 Þ 2 as well as a number of features that may be attributable to a wide range of mono-and polyhydrated sulphates and hydroxyl-sulphates bearing a number of cations, including Mg 2+ , Fe 2+ , Fe 3+ and Ca 2+ . Spectral features similar to those of ammonium sulphates may also be present.Analysis of a HiRISE stereo DEM shows planar layering in some ILDs, favouring a sedimentary deposition origin. Stratigraphic mapping of hydration and sulphate spectral features in flat ILDs in central Iani Chaos suggest that specific elevation intervals in the stratigraphic column were subject to different levels of hydration, perhaps during episodes of water table elevation. This is consistent with formation models for ILDs and hydrological modelling. Geomorphic characteristics of deposits in northern and southern Iani Chaos suggest their relatively recent exhumation and significant erosion by aeolian processes. We conclude that any formation theory for ILDs in Iani Chaos should support mechanisms for different hydration states at different stratigraphic elevations and subsequent significant aeolian erosion, burial and reexposure.

show abstract

Section: Ilds In Iani Chaosmentioning

confidence: 99%

Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars

Sefton‐Nash

Catling

Wood

et al. 2012

Icarus

View full text Add to dashboard Cite

show abstract

“…However, the nature of the oxidant responsible for the evolution of the oxidation state of the surface is still unknown. Photodissociation of H 2 O and further thermal escape of H 2 are efficient mechanisms to produce O 2 which equilibrates with the primary hydrosphere and oxidizes Fe 2+ precursors into ferric (oxy)hydroxides (Catling and Moore, 2003;Lammer et al, 2003). However, some calculations have shown that O 2 would have always remained a trace component of the martian atmosphere (Catling and Moore, 2003).…”

Section: Weathering Model and Evolution Of Martian Surface Conditionsmentioning

confidence: 99%

“…Alternatively, the direct transformation of goethite to hematite may be promoted by high temperature. A possible origin to the layers of ''grey crystalline hematite'' observed by TES onboard Mars Global Surveyor (Christensen et al, 2000;Hynek et al, 2002) and for Maridiani Planum ''blueberries'' is through burial and subsequent thermal recrystallization of basaltic rocks previously altered by water (Catling and Moore, 2003;Christensen and Ruff, 2004). Laboratory experiments show that the best precursor for the hematite spectra is goethite heated to about 300°C (Glotch et al, 2004).…”

Section: Evolution Of Iron (Oxy)hydroxides On Marsmentioning

confidence: 99%

“…The large formations of ''grey crystalline hematite'' discovered by Mars Odyssey (Christensen et al, 2000;Hynek et al, 2002) have various possible origins, including precipitation from a low-temperature aqueous phase, burial or thermal metamorphism favoured by hydrothermalism, deuteritic alteration of lava, weathering processes etc. (Christensen et al, 2001;Catling and Moore, 2003;Baldridge and Calvin, 2004;Christensen and Ruff, 2004). Mars Exploration Rover (MER) Opportunity has provided evidence for the past presence of water in Meridiani Planum by the observation of sedimentary layers containing jarosite ((H 3 O + , K + )Fe 3þ 3 (SO 4 ) 2 (OH) 6 ) and spherical aggregates of crystalline hematite, so called ''blueberries' ' (Klingelhöfer et al, 2004).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Iron weathering products in a CO2+(H2O or H2O2) atmosphere: Implications for weathering processes on the surface of Mars

Chevrier

Mathé

Rochette

et al. 2006

Geochimica et Cosmochimica Acta

View full text Add to dashboard Cite

“…Hematite photochemical properties, including anisotropic properties, may also be key to understanding the long-term evolution of Mars surface. It is known that hematite on Mars exhibits preferential orientation, with (001) facets preferentially exposed at the surface (Catling and Moore, 2003).…”

Section: Introductionmentioning

confidence: 99%

Anisotropic photocatalytic properties of hematite

et al. 2009

View full text Add to dashboard Cite

Hematite is a semiconducting mineral with a role in natural photoelectrochemical processes, and has been studied from the viewpoint of solar energy utilization. Hematite is an anisotropic conductor, with faster conduction parallel to (001) planes. Flatband potentials and photocurrent onset potentials for natural hematite single crystals and synthetic nanocrystalline hematite films are similar, and show Nernstian behavior within error. At pH 7, the flatband potential of single crystals is -0.25AE0.1 V vs. Ag/AgCl. Photocurrent onset potential is 0.02 to 0.03 V more negative for crystal faces than for crystal edges. Photocurrent density is a factor of 5 to 10 higher for crystal edges than for crystal (001) faces, presumably because of more rapid charge separation for the edges. Falling photocurrent transients decay more slowly for edges than for faces, consistent with more rapid removal of conduction band electrons into the bulk and therefore reduced availability of such electrons for back reaction. Rising photocurrent transients occur at higher potential, and have the same rise time for both faces and edges. This suggests that the rising transients are due to slow conduction through bulk hematite. The transition from falling to rising transients occurs at a more positive potential for edges than for faces, which is also consistent with more rapid charge transport away from edge surfaces and with Fermi level pinning at edges.

show abstract

The nature of coarse-grained crystalline hematite and its implications for the early environment of Mars

Cited by 147 publications

References 111 publications

Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars

Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars

Iron weathering products in a CO2+(H2O or H2O2) atmosphere: Implications for weathering processes on the surface of Mars

Anisotropic photocatalytic properties of hematite

Contact Info

Product

Resources

About