Transmission infrared spectra (2–25μm) of carbonaceous chondrites (CI, CM, CV–CK, CR, C2 ungrouped): Mineralogy, water, and asteroidal processes

Beck, Pierre; Garenne, A.; Quirico, E.; Bonal, L.; Montes-Hernandez, German; Moynier, Frédéric; Schmitt, Bernard

doi:10.1016/j.icarus.2013.10.019

Cited by 122 publications

(186 citation statements)

References 104 publications

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“…The main features in the spectra for Ivuna and Orgueil are a peak at~9.9 μm and a doublet at~23 μm from the Si-O stretching and bending modes, which we attribute to the abundant phyllosilicates present in these meteorites. The position of the 10-μm feature best matches the saponite standard, in agreement with the findings of Beck et al (2014a). Our data are also similar to the reflectance mid-IR spectra of McAdam et al (2015), who suggested that Orgueil is dominated by a Mg-rich trioctahedral phyllosilicate.…”

Section: Quantifying H 2 Osupporting

confidence: 90%

“…Ivuna and Orgueil display the sharp peak at~2.71 μm due to bound -OH ions, whereas it is almost absent from Y-82162 and Y-980115. A noticeable reduction in the intensity of the 3-μm feature is a common characteristic of thermally altered carbonaceous chondrites (Sato et al 1997;Osawa et al 2005;Beck et al 2014a Orgueil of 17.4 wt.%. Their abundance is slightly lower than ours as they only take into account mass loss from 200 to 770°C and suggest that everything above this temperature is carbonate decomposition.…”

Section: Ir Spectroscopymentioning

confidence: 97%

“…However, to minimise the effects of adsorbed water (e.g. Beck et al 2010Beck et al , 2014a, we repeated the measurements after drying them at 300°C for 2 h. Figure 1 shows the DTG (wt.%/°C) curves for the phyllosilicate, Fe-(oxy)hydroxide and carbonate standard minerals. The DTG curve shows how the weight of the sample changes during heating.…”

Section: Ir Spectroscopymentioning

confidence: 99%

“…There has been a move towards resolving differences in the relative extent of aqueous alteration in carbonaceous chondrites using bulk H contents (Alexander et al 2013), total phyllosilicate abundances (Howard et al 2009(Howard et al , 2011 and IR spectral features (Beck et al 2010(Beck et al , 2014aMcAdam et al 2015). In general, good agreement is found between alteration scales determined using these methods.…”

Section: Degree Of Aqueous Alterationmentioning

confidence: 99%

“…Here, we have taken aliquots of the same powders and characterised them using thermogravimetric analysis (TGA) and infrared (IR) spectroscopy. Recent work by Beck et al (2010Beck et al ( , 2014a and Garenne et al (2014) demonstrated that combined TGA and IR datasets can be used to examine the bulk mineralogy and quantify the abundance of H 2 O in carbonaceous chondrites, providing useful insights into the nature and extent of aqueous and thermal alteration. Our results show that at the bulk scale, CI chondrites experienced essentially the same degree of aqueous alteration, in agreement with the findings of King et al (2015).…”

Section: Introductionmentioning

confidence: 99%

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Characterising the CI and CI-like carbonaceous chondrites using thermogravimetric analysis and infrared spectroscopy

et al. 2015

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The CI and CI-like chondrites provide a record of aqueous alteration in the early solar system. However, the CI-like chondrites differ in having also experienced a late stage period of thermal metamorphism. In order to constrain the nature and extent of the aqueous and thermal alteration, we have investigated the bulk mineralogy and abundance of H 2 O in the CI and CI-like chondrites using thermogravimetric analysis and infrared spectroscopy. The CI chondrites Ivuna and Orgueil show significant mass loss (28.5-31.8 wt.%) upon heating to 1000°C due to dehydration and dehydroxylation of abundant phyllosilicates and Fe-(oxy)hydroxides and the decomposition of Fe-sulphides, carbonates and organics. Infrared spectra for Ivuna and Orgueil have a prominent 3-μm feature due to bound −OH/H 2 O in phyllosilicates and Fe-(oxy)hydroxides and only a minor 11-μm feature from anhydrous silicates. These characteristics are consistent with previous studies indicating that the CI chondrites underwent near-complete aqueous alteration. Similarities in the total abundance of H 2 O and 3 μm/11 μm ratio suggest that there is no difference in the relative degree of hydration experienced by Ivuna and Orgueil. In contrast, the CI-like chondrites Y-82162 and Y-980115 show lower mass loss (13.8-18.8 wt.%) and contain >50 % less H 2 O than the CI chondrites. The 3-μm feature is almost absent from spectra of Y-82162 and Y-980115 but the 11-μm feature is intense. The CI-like chondrites experienced thermal metamorphism at temperatures >500°C that initially caused dehydration and dehydroxylation of phyllosilicates before partial recrystallization back into anhydrous silicates. The surfaces of many C-type asteroids were probably heated through impact metamorphism and/or solar radiation, so thermally altered carbonaceous chondrites are likely good analogues for samples that will be returned by the Hayabusa-2 and OSIRIS-REx missions.

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Section: Quantifying H 2 Osupporting

confidence: 90%

Section: Ir Spectroscopymentioning

confidence: 97%

Section: Ir Spectroscopymentioning

confidence: 99%

Section: Degree Of Aqueous Alterationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Characterising the CI and CI-like carbonaceous chondrites using thermogravimetric analysis and infrared spectroscopy

et al. 2015

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Water in the Martian regolith from OMEGA/Mars Express

Audouard

Poulet

Vincendon

et al. 2014

J. Geophys. Res. Planets

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Here we discuss one of the current reservoirs of water on Mars, the regolith and rocks exposed at the surface. This reservoir is characterized by the presence of H 2 O-and OH-bearing phases that produce a broad absorption at a wavelength of~3 μm in near-infrared (NIR) reflectance spectra. This absorption is present in every ice-free spectrum of the Martian surface obtained thus far by orbital NIR spectrometers. We present a quantitative analysis of the global distribution of the 3 μm absorption using the Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité (OMEGA) imaging spectrometer that has been mapping the surface of Mars at kilometer scale for more than 10 years. Based on laboratory reflectance spectra of a wide range of hydrous minerals and phases, we estimate a model-dependent water content of 4 ± 1 wt % in the equatorial and midlatitudes. Surface hydration increases with latitude, with an asymmetry in water content between the Northern and Southern Hemispheres. The surface hydration is compared to various parameters (albedo, dust, geological units, time, relative humidity, atmospheric water pressure, and in situ measurements performed by Phoenix and Curiosity) to constrain the nature of the reservoir. We conclude that the nature of the surface hydration of the Martian low latitudes is not adsorbed water but rather more tightly bound water molecules and hydroxyl groups in the structure of the materials of the near-top surface. A frost-related process best explains the implementation of water into and onto the first microns of the high-latitude Martian regolith.

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Sample return of primitive matter from the outer Solar System

et al. 2021

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The last thirty years of cosmochemistry and planetary science have shown that one major Solar System reservoir is vastly undersampled in the available suite of extra-terrestrial materials, namely small bodies that formed in the outer Solar System (>10 AU). Because various dynamical evolutionary processes have modified their initial orbits (e.g., giant planet migration, resonances), these objects can be found today across the entire Solar System as P/D near-Earth and main-belt asteroids, Jupiter and Neptune Trojans, comets, Centaurs, and small (diameter < 200 km) trans-Neptunian objects. This reservoir is of tremendous interest, as it is recognized as the least processed since the dawn of the Solar System and thus the closest to the starting materials from which the Solar System formed. Some of the next major breakthroughs in planetary science will come from studying outer Solar System samples (volatiles and refractory constituents) in the laboratory. Yet, this can only be achieved by an L-class mission that directly collects and returns to Earth materials from this reservoir. It is thus not surprising that two White Papers advocating a sample return mission of a primitive Solar System small body (ideally a comet) were submitted to ESA in response to its Voyage 2050 call for ideas for future L-class missions in the 2035-2050 time frame. One of these two White Papers is presented in this article.

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Transmission infrared spectra (2–25μm) of carbonaceous chondrites (CI, CM, CV–CK, CR, C2 ungrouped): Mineralogy, water, and asteroidal processes

Cited by 122 publications

References 104 publications

Characterising the CI and CI-like carbonaceous chondrites using thermogravimetric analysis and infrared spectroscopy

Characterising the CI and CI-like carbonaceous chondrites using thermogravimetric analysis and infrared spectroscopy

Water in the Martian regolith from OMEGA/Mars Express

Sample return of primitive matter from the outer Solar System

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