Thermal history of type 3 chondrites from the Antarctic meteorite collection determined by Raman spectroscopy of their polyaromatic carbonaceous matter

Bonal, L.; Quirico, E.; Flandinet, Laurène; Montagnac, Gilles

doi:10.1016/j.gca.2016.06.017

Cited by 89 publications

(183 citation statements)

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“…A variety of other observations, including Raman spectroscopy of the organic component of these two CO meteorites, have recently confirmed that they are indeed very primitive (Bonal et al. ; Alexander et al. ).…”

Section: Introductionmentioning

confidence: 82%

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Distribution of aliphatic amines in CO, CV, and CK carbonaceous chondrites and relation to mineralogy and processing history

Aponte

Abreu

Glavin

et al. 2017

Meteorit & Planetary Scien

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The analysis of water‐soluble organic compounds in meteorites provides valuable insights into the prebiotic synthesis of organic matter and the processes that occurred during the formation of the solar system. We investigated the concentration of aliphatic monoamines present in hot acid water extracts of the unaltered Antarctic carbonaceous chondrites, Dominion Range (DOM) 08006 (CO3) and Miller Range (MIL) 05013 (CO3), and the thermally altered meteorites, Allende (CV3), LAP 02206 (CV3), GRA 06101 (CV3), Allan Hills (ALH) 85002 (CK4), and EET 92002 (CK5). We have also reviewed and assessed the petrologic characteristics of the meteorites studied here to evaluate the effects of asteroidal processing on the abundance and molecular distributions of monoamines. The CO3, CV3, CK4, and CK5 meteorites studied here contain total concentrations of amines ranging from 1.2 to 4.0 nmol g−1 of meteorite; these amounts are 1–3 orders of magnitude below those observed in carbonaceous chondrites from the CI, CM, and CR groups. The low‐amine abundances for CV and CK chondrites may be related to their extensive degree of thermal metamorphism and/or to their low original amine content. Although the CO3 meteorites, DOM 08006 and MIL 05013, do not show signs of thermal and aqueous alteration, their monoamine contents are comparable to those observed in moderately/extensively thermally altered CV3, CK4, and CK5 carbonaceous chondrites. The low content of monoamines in pristine CO carbonaceous chondrites suggests that the initial amounts, and not asteroidal processes, play a dominant role in the content of monoamines in carbonaceous chondrites. The primary monoamines, methylamine, ethylamine, and n‐propylamine constitute the most abundant amines in the CO3, CV3, CK4, and CK5 meteorites studied here. Contrary to the predominance of n‐ω‐amino acid isomers in CO3 and thermally altered meteorites, there appears to be no preference for the larger n‐amines.

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Section: Introductionmentioning

confidence: 82%

“…Multiple studies have demonstrated that organic materials in CV meteorites progressively mature as a result of thermal metamorphism and that there is a correlation between carbonization of organics and the mineralogical characteristics of matrices (e.g., Brearley ; Abreu and Brearley ; Bonal et al. , ; Le Guillou et al. ).…”

Section: Discussionmentioning

confidence: 99%

Distribution of aliphatic amines in CO, CV, and CK carbonaceous chondrites and relation to mineralogy and processing history

Aponte

Abreu

Glavin

et al. 2017

Meteorit & Planetary Scien

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“…Γ D has been reported to be more sensitive to metamorphism than Γ G ; therefore, it is expected to reflect the thermal history of the parent asteroid more accurately than Γ G does. In Figure (bottom), the Γ D has a positive correlation with Γ D /Γ G , showing the dependence (spread) of the D band to the thermal maturity of carbon as expected (e.g., Bonal et al). On the other hand, Γ G presents a negative correlation.…”

Section: Resultsmentioning

confidence: 99%

“…Raman spectral parameters have previously been reported for various types of meteorites in an effort to understand parent body thermal histories . For instance, Raman spectra of the first order carbon bands in the UOC, CO, and CV samples were collected using a 514.5‐nm laser, and the D and G band parameters were extracted using Lorentzian and Breit‐Wigner‐Fano fit functions, respectively . Figure presents comparison of first order carbon spectral peak parameters of ALHA77278 with meteorites of different types and petrologic grades.…”

Section: Resultsmentioning

confidence: 99%

“…This is especially useful for meteorites where various chemical materials of interest may not be present on the surface but at an unknown depth in the sample. In addition, spectral peak parameters of carbon structures are often used to infer thermal metamorphic history of samples (e.g., Bonal et al). In the case of thin sections, carbon phases that are on the surface of samples may be modified during sample preparation .…”

Section: Resultsmentioning

confidence: 99%

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Investigation of carbon in the Allan Hills A77278 meteorite via 2D and 3D Raman microspectroscopy

Yeşiltaş

2018

J Raman Spectroscopy

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This paper reports the first Raman spectral and imaging data on the ordinary chondrite Allan Hills A77278 (ALHA77278) in two and three dimensions. Mineralogy in the ALHA77278 meteorite appears to be mainly silicates (olivine and pyroxene) with some carbonaceous material in the matrix. Metal phases are also present in the studied sample. Two‐dimensional Raman spectral distribution maps show the locations of these chemical constituents. Several diamond grains are observed to be buried in olivine and extend down to a ~7‐μm depth in the sample, which might be contamination captured during the sample preparation. Raman spectral peak parameters for D and G carbon bands are presented and trends among these parameters are discussed. These spectral parameters, when compared with those of other meteorites reported in the literature, show similarity with unequilibrated ordinary chondrites and primitive carbonaceous chondrites. Estimated peak metamorphic temperature for the parent asteroid is calculated to be around ~260°C, which is comparable with lower metamorphic grade ordinary chondrites, indicating that the metamorphic grade of ALHA77278 might be less than 3.7, as it has been officially assigned. Three‐dimensional Raman tomographic measurements present visualizations of the identified chemical components in high resolution as well as the epoxy used during the preparation of the sample. Spatial distribution of epoxy is used to avoid these regions during the Raman spectral data extraction from the carbonaceous matter from a depth of the sample, which could otherwise complicate the datasets used to infer the thermal history of the ALHA77278 meteorite.

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Calibration of Raman wavenumber in large Raman images using a mercury‐argon lamp

Jakubek

Fries

2020

J Raman Spectroscopy

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Raman imaging is an emerging tool for the analysis of meteorites, as it is capable of describing mineralogy, carbon composition/speciation, and crystal orientation all within a petrographic context. Adequately examining the heterogeneous composition of a meteorite often requires long image collection times on the timescale of days. However, the wavenumber calibration of the Raman spectrometer drifts over long timescales resulting in low wavenumber precision for the Raman spectra comprising a large Raman image. This decrease in wavenumber precision can compromise the analysis of geological markers that can provide important information on a meteorite sample. We examine, in detail, the change in bandwidth and wavenumber of the Raman bands and Hg–Ar emission lines in our Raman images as a function of time and laboratory temperature. To overcome the drift in calibration, we utilize a commercial WITec Raman instrument with a built‐in Hg–Ar calibration lamp to individually calibrate each spectrum in the Raman image. We show that using the Hg–Ar calibration, we can improve the wavenumber precision for the spectra in our Raman images from ~±0.15 to ~±0.05 cm−1 for Raman spectra collected over multiple days. This is important as it improves measurements of mineral chemistry, latent strain, and other features that are dependent upon accurate peak position determination. We also examine the spectral signal‐to‐noise ratio needed to minimize the wavenumber error when fitting bands to Gaussian/Lorentzian profiles. We then use our results to suggest a general method for calibrating the wavenumber of Raman spectra in large Raman images.

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Thermal history of type 3 chondrites from the Antarctic meteorite collection determined by Raman spectroscopy of their polyaromatic carbonaceous matter

Cited by 89 publications

References 54 publications

Distribution of aliphatic amines in CO, CV, and CK carbonaceous chondrites and relation to mineralogy and processing history

Distribution of aliphatic amines in CO, CV, and CK carbonaceous chondrites and relation to mineralogy and processing history

Investigation of carbon in the Allan Hills A77278 meteorite via 2D and 3D Raman microspectroscopy

Calibration of Raman wavenumber in large Raman images using a mercury‐argon lamp

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