The Meteoritical Bulletin, No. 109

Gattacceca, J.; McCubbin, F. M.; Grossman, J. N.; Bouvier, Audrey; Bullock, E. S.; Aoudjehane, Hasnaa Chennaoui; Debaille, Vinciane; D’Orazio, Massimo; Komatsu, M.; Miao, Bingkui; Schrader, D. L.; Jull, A. J. T.

doi:10.1111/maps.13714

Cited by 30 publications

(23 citation statements)

References 18 publications

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“…Thus, the order of hydration obtained by TGA is as follows: CI1 (Orgueil) > Tarda % Tagish Lake % CR1(GRO 95577) ≥ CM2 (Aguas Zarcas and Murchison) > heated CM2 (Jbilet Winselwan and ALH 84033). Raman D and G band parameters of Tarda and Tagish Lake are consistent as well and indicate highly 2010), CO data are from Greenwood and Franchi (2004), AZ data are from Meteoritical Bulletin 108 (Gattacceca et al, 2021), EET 83226 and C3-ung data are from Torrano et al (2021), and Zag data are from Zolensky et al (2003) and Kebukawa, Alexander, et al (2019) and Kebukawa, Ito, et al (2019). disordered carbon due to minimal thermal metamorphism.…”

Section: Hydrated Versus Less Hydrated Meteoritesmentioning

confidence: 65%

“…(2014); CV and CK data are from Greenwood et al. (2010), CO data are from Greenwood and Franchi (2004), AZ data are from Meteoritical Bulletin 108 (Gattacceca et al., 2021), EET 83226 and C3‐ung data are from Torrano et al. (2021), and Zag data are from Zolensky et al.…”

Section: Discussionmentioning

confidence: 99%

“…CCAM, carbonaceous chondrite anhydrous mineral line. Data for Tarda are from Meteoritical Bulletin 109 (Gattacceca et al, 2020); CM, CR, CI, CY, Allende, and C2-ung data are from Clayton and Mayeda (1999) and Tonui et al (2014); CV and CK data are from Greenwood et al (2010), CO data are fromGreenwood and Franchi (2004), AZ data are from Meteoritical Bulletin 108(Gattacceca et al, 2021), EET 83226 and C3-ung data are fromTorrano et al (2021), and Zag data are fromZolensky et al (2003) andKebukawa, Alexander, et al (2019) andKebukawa, Ito, et al (2019).…”

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confidence: 99%

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Compositional and spectroscopic investigation of three ungrouped carbonaceous chondrites

Yeşiltaş

Kebukawa

Glotch

et al. 2022

Meteorit & Planetary Scien

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Ungrouped carbonaceous chondrites are not easily classified into one of the well‐established groups due to compositional/petrological differences and geochemical anomalies. Type 2 ungrouped carbonaceous chondrites represent a very small fraction of all carbonaceous chondrites. They can potentially represent different aspects of asteroids and their regolith material. By conducting a multitechnique investigation, we show that Queen Alexandra Range (QUE) 99038 and Elephant Moraine (EET) 83226 do not resemble type 2 carbonaceous chondrites. QUE 99038 exhibits coarse‐grained matrix, Fe‐rich rims on olivines, and an apparent lack of tochilinite, suggesting that QUE 99038 has been metamorphosed. Its polyaromatic organic matter structures closely resemble oxidized CV3 chondrites. EET 83226 exhibits a clastic texture with high porosity and shows similarities to CO3 chondrites. It consists of numerous large chondrules with fine‐grained rims that are often fragmented and discontinuous and set within matrix, suggesting a formation mechanism for the rims in a regolith environment. The kind of processes that can result in such chemical compositions as in QUE 99038 and EET 83226 is currently not fully known and clearly presents a conundrum. Tarda is a highly friable carbonaceous chondrite with close resemblance to Tagish Lake (ungrouped C2 chondrite). It comprises different types of chondrules (some with Fe‐rich rims), framboid magnetite, sulfides, carbonates, and phyllosilicate‐ and carbon‐rich matrix, and is consistent with being an ungrouped C2 chondrite.

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Section: Hydrated Versus Less Hydrated Meteoritesmentioning

confidence: 65%

Section: Discussionmentioning

confidence: 99%

mentioning

confidence: 99%

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Compositional and spectroscopic investigation of three ungrouped carbonaceous chondrites

Yeşiltaş

Kebukawa

Glotch

et al. 2022

Meteorit & Planetary Scien

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“…Currently, the most altered CM fall is Kolang (CM2.2), which landed in Indonesia in 2020 (King et al, 2021), and also contains CM1 clasts (Schrader et al, 2021). The new Winchcombe CM2 fall is also very highly aqueously altered, containing CM1/2 and CM1 lithologies (Gattacceca et al, 2021). CM1 meteorites can be either friable or brittle.…”

Section: CMmentioning

confidence: 99%

Abundance and importance of petrological type 1 chondritic material

Russell

Suttle

King

2021

Meteorit & Planetary Scien

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We review the mineralogy, petrology, and abundance of petrological type 1 extraterrestrial material. Such material has been completely altered by aqueous processing on its parent bodies. As well as the four meteorite groups that contain type 1 members (CI, CM, CR, and CY), we summarize data from the 2019 fall Flensburg and a recent reanalysis of the "meteorite" Bench Crater found on the Moon, along with fine-grained micrometeorites, interplanetary dust particles, and xenoliths in meteorites. Type 1 materials exhibit a remarkably high diversity of alteration conditions (temperature, water-to-rock [W/R] ratios, and fluid composition) and starting mineralogy. Type 1 material comprises a significant component of the modern extraterrestrial flux to the Earth and was likely common throughout the solar system during the whole course of its history, pointing to both widespread accretion with ices and heating of parent bodies. Type 1 materials are composed predominantly of various phyllosilicates, carbonates, sulfides, and magnetite. Some type 1 materials appear to be part of a "CM clan" typified by serpentine-rich phyllosilicate compositions and an oxygen isotope composition that falls in the 16 O-rich part of the CM field. Others span a wide range in d 18 O (>30&) and fall on or above the terrestrial fractionation line (+ve D 17 O). Positive D 17 O values are unusual for carbonaceous meteorites but are relatively common in type 1 materials. The wide variation in oxygen isotopes, as well as in textures, mineralogy, and bulk chemistry, points to multiple parent bodies that may originate in the inner and/or outer solar system. Cometary materials, or transition objects such as Main Belt comets or type D asteroids, are likely the source of much of the type 1 materials on Earth but relating them to specific parents requires more study.

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“…Martian meteorites are the only samples from the Red Planet available for laboratory analyses. More than 307 pieces of 166 unique samples, originating from at least 11 source craters, are curated in the world’s collections 1 . Ejection ages, based on cosmic ray exposure (CRE), vary from 0.7 to 20 Myr 2 – 4 .…”

Section: Introductionmentioning

confidence: 99%

The Tharsis mantle source of depleted shergottites revealed by 90 million impact craters

et al. 2021

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The only martian rock samples on Earth are meteorites ejected from the surface of Mars by asteroid impacts. The locations and geological contexts of the launch sites are currently unknown. Determining the impact locations is essential to unravel the relations between the evolution of the martian interior and its surface. Here we adapt a Crater Detection Algorithm that compile a database of 90 million impact craters, allowing to determine the potential launch position of these meteorites through the observation of secondary crater fields. We show that Tooting and 09-000015 craters, both located in the Tharsis volcanic province, are the most likely source of the depleted shergottites ejected 1.1 million year ago. This implies that a major thermal anomaly deeply rooted in the mantle under Tharsis was active over most of the geological history of the planet, and has sampled a depleted mantle, that has retained until recently geochemical signatures of Mars’ early history.

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The Meteoritical Bulletin, No. 109

Cited by 30 publications

References 18 publications

Compositional and spectroscopic investigation of three ungrouped carbonaceous chondrites

Compositional and spectroscopic investigation of three ungrouped carbonaceous chondrites

Abundance and importance of petrological type 1 chondritic material

The Tharsis mantle source of depleted shergottites revealed by 90 million impact craters

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