Sulfates in Martian Layered Terrains: The OMEGA/Mars Express View

By A. Gendrin, Nicolas Mangold, J. Bibring, Yves Langevin, B. Gondet, François Poulet, G. Bonello, C. Quantin, J. F. Mustard, R. Arvidson and 1 more. Science, 2005

1,006 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/ea6ad075fb49cd9e4a4e486aed890f37cd66111c

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Citations in the corpus

The sulfur content of volcanic gases on Mars (2009, background): “…instruments on spacecrafts sent to Mars have shown the martian regolith to be uniformly rich in sulfur, in the sulfate form ([Yen, 2005] and [Gendrin et al., 2005]), with abundances typically exceeding 2 orders of magnitude those of common sedimentary or igneous rocks on Earth ([Yen, 2005]…”
Mineralogy and evolution of the surface of Mars: A review (2007, background): “The layered terrains containing the sulphates represent important deposits, tens of km wide, and with a thickness of a few km (Bibring et al., 2005; Gendrin et al., 2005).”
Formation of recurring slope lineae by liquid brines on present‐day Mars (2012, background): “However, if the RSL are indeed formed by brines, it may indicate that a recharge mechanism is active in order to maintain a source of brine over even short geological timescales, which would have important implications for the Martian water cycle.”
The Sedimentary Rock Record of Mars: Distribution, Origins, and Global Stratigraphy (2012, methodology): “Phyllosilicates are most commonly found in Noachian-age terrains, sulfates are primarily associated with younger Hesperian terrains, and anhydrous Fe-oxides are dominant in Amazonian terrains; Bibring et al. (2006) refer to these ‘‘mineralogical’’ time periods as the phyllosian, theiikian, and sider”
Concentration of H, Si, Cl, K, Fe, and Th in the low- and mid-latitude regions of Mars (2007, methodology): “These have included Earth-based observational programs using reflectance spectroscopy [e.g., Singer et al., 1979; Mere´nyi et al., 1996a, 19996b], and more recently, orbital studies at regional to global scales carried out using visible and infrared imaging [e.g., Bandfield et al., 2000; Christensen”
Quantifying absolute water content of minerals using near‐infrared reflectance spectroscopy (2005, background): “…absorptions near 1.9 mm and absolute water content that is independent of composition or between these absorptions and their counterparts near 2.9–3.1 mm. Combination overtone absorptions near 1.9 mm therefore are not expected to be reliable estimators of water content for mixtures of minerals.”
A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter (2009, background): “Groups of strata contain dispersed crystalline ferric oxide, which is concentrated in talus [Gendrin et al., 2005b; Bibring et al., 2007; Mangold et al., 2008; Le Deit et al., 2007; Murchie et al., 2009b].”
Exploration of hydrothermal targets on Mars (2007, methodology): “Sulfates in Martian Layered Terrains: The OMEGA/Mars Express View.”
Mineralogy of the Martian Surface (2014, background): “Subsequently, orbital VNIR imaging showed that the Hesperian sedimentary rocks with hematite and polyhydrated and monohydrated sulfates overlie Noachian units with clays (Gendrin et al. 2005; Arvidson et al. 2005, 2006; Wiseman et al. 2010).”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, background): “(Gendrin et al., 2005; Squyres and Knoll, 2005; Halevy et al., 2007). Johnson et al. (2008) investigated the impact of larger amount of”
Geologic Constraints on Early Mars Climate (2018, background): “Rock-making probably involves cementation by aqueous minerals (Gendrin et al. 2005, Murchie et al. 2009, Grotzinger & Milliken 2012, McLennan et al. 2019).”