Signatures of the post-hydration heating of highly aqueously altered CM carbonaceous chondrites and implications for interpreting asteroid sample returns

Lindgren, P.; Lee, Martin; Sparkes, R.; Greenwood, Richard C.; Hanna, R. D.; Franchi, I. A.; King, A. J.; Floyd, Cameron; Martin, Pierre Etienne; Hamilton, Victoria E.; Haberle, C. W.

doi:10.1016/j.gca.2020.08.021

Cited by 17 publications

(18 citation statements)

References 101 publications

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“…The mass loss for LAP 04514 between 300 and 450 °C is higher than that observed for CM chondrites heated to Stage II (300–500 °C) (King et al., 2021; Nakamura, 2005), while, as described above, we still detect Fe‐serpentine peaks in its XRD pattern. We therefore estimate that the peak metamorphic temperature for LAP 04514 was ~300–400 °C, although CM chondrites heated to the upper end of that range (e.g., 400 °C) for short periods of time (e.g., 24 h) can also show coherent diffraction from Fe‐serpentine (Lindgren et al., 2020).…”

Section: Discussionmentioning

confidence: 99%

“…XRD is sensitive to the collapse of phyllosilicate structures that occurs during dehydration. XRD patterns of naturally and artificially heated CM chondrites lack coherent phyllosilicate diffraction peaks after heating at temperatures > ~300–400 °C (King et al., 2021; Lindgren et al., 2020; Nakamura, 2005; Tonui et al., 2014). For LAP 04796, LAP 04565, and LAP 02333, we observe typical diffraction peaks from Fe‐ and Mg‐rich serpentines, indicating that these meteorites were not heated to > ~300–400 °C after aqueous alteration had ceased (Fig.…”

Section: Discussionmentioning

confidence: 99%

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Tracing the earliest stages of hydrothermal alteration on the CM chondrite parent body

King

Mason

Bates

et al. 2021

Meteorit & Planetary Scien

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The CM carbonaceous chondrites are an important resource in our efforts to understand the role of volatiles in the formation of planetary systems. We report the bulk mineralogy, water abundance, and infrared (IR) reflectance spectra of the CM chondrites LaPaz Icefield (LAP) 04514, LAP 04796, LAP 04565, and LAP 02333. They contain abundant Fe‐ and Mg‐rich serpentines (~70–80 vol%), and based on their phyllosilicate fractions, we classify LAP 04514, LAP 04796, and LAP 04565 as petrologic subtype 1.6 and LAP 02333 as 1.4. This is consistent with estimated water abundances of 9.9 (±1.1) wt% for LAP 04796, 10.4 (±0.1) wt% for LAP 04565, and 11.5 (±0.5) wt% for LAP 02333. However, LAP 04514 contains less water (8.8 ± 0.3 wt%), has a shallower 3 µm band depth, and lacks tochilinite having experienced posthydration temperatures of ~300–400 °C. We conclude that LAP 04514, LAP 04796, and LAP 04565 are among the least altered CM chondrites, which retain primitive features from the initial building blocks of the CM parent body. Finally, we use the IR spectral features of LAP 04514, LAP 04796, and LAP 04565 to identify C‐complex asteroid surfaces that record mild levels of hydration.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Tracing the earliest stages of hydrothermal alteration on the CM chondrite parent body

King

Mason

Bates

et al. 2021

Meteorit & Planetary Scien

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“…This assumption is reasonable as phyllosilicates are known to produce an amorphous material upon heating (e.g. Akai 1992;Gualtieri et al 2012;Lindgren et al 2020) and petrographic evidence supports their presence in the Stage II meteorites. Primary amorphous silicates and rusts could occur, but their contribution to the bulk mineralogy is relatively minor.…”

Section: Degree Of Aqueous Alterationmentioning

confidence: 92%

“…4 He and 20 Ne) (Nakamura 2006), and volatile trace elements (e.g. Cd) (Paul and Lipschutz 1990;Xiao and Lipschutz 1992; Wang and Lipschutz 1998;Lipschutz et al 1999), while oxygen isotopic compositions can be shifted (Clayton and Mayeda 1999;Lindgren et al 2020) and organics modified or destroyed (Kitajima et al 2002;Quirico et al 2018;Chan et al 2019). By studying these different properties, and through comparison to the products of artificial heating experiments, it has been shown that some CM chondrites suffered relatively mild thermal metamorphism at temperatures of <500°C, whereas others were fully dehydrated and recrystallised at >750°C (Nakamura 2005;Tonui et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Thermal alteration of CM carbonaceous chondrites: Mineralogical changes and metamorphic temperatures

King

Schofield

Russell

2021

Geochimica et Cosmochimica Acta

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“…Clayton and Mayeda (1999) suggested that CY meteorites may have been derived from CI meteorites from such a process. Ivanova et al (2013), working on analog material, found that isotopic fractionation to higher d 18 O compositions occurred during dehydration and Lindgren et al (2020) reported similar effects. However, Clayton and Mayeda (1999) artificially heated CI and CM meteorites and found both heavier and lighter compositions were produced.…”

Section: Oxygen Isotopesmentioning

confidence: 82%

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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Signatures of the post-hydration heating of highly aqueously altered CM carbonaceous chondrites and implications for interpreting asteroid sample returns

Cited by 17 publications

References 101 publications

Tracing the earliest stages of hydrothermal alteration on the CM chondrite parent body

Tracing the earliest stages of hydrothermal alteration on the CM chondrite parent body

Thermal alteration of CM carbonaceous chondrites: Mineralogical changes and metamorphic temperatures

Abundance and importance of petrological type 1 chondritic material

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