The aqueous alteration of CM chondrites, a review

Suttle, M. D.; King, A. J.; Schofield, P. F.; Bates, H. C.; Russell, S. S.

doi:10.1016/j.gca.2021.01.014

Cited by 55 publications

(83 citation statements)

References 285 publications

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“…This is attested by the ubiquitous occurrence of brecciated textures in meteorites, with~30% of ordinary chondrites (OCs) and almost all CM carbonaceous chondrites showing brecciation features (Fig. 1A) (Bischoff et al 2006;Gattacceca et al 2017;Lentfort et al 2021;Suttle et al 2021). Such characteristics are fundamental because (1) OCs are by far the most common meteorites falling on Earth (~80%) and (2) CMs represent 25% of all carbonaceous chondrite falls (Gounelle et al 2005).…”

Section: Meteoritic Evidence Of Widespread Collision Processes In the Asteroid Beltmentioning

confidence: 98%

The astrophysical context of collision processes in meteorites

Marrocchi

Delbò

Gounelle

2021

Meteorit & Planetary Scien

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Chondrites are leftover solids from the early evolution of the solar protoplanetary disk that never experienced melting since their formation. They comprise unequilibrated assemblages of low-and high-temperature components, including volatile-rich, fine-grained matrices, Fe-Ni metal, sulfides, refractory inclusions, and chondrules. Consequently, chondrites are commonly described as pristine, primitive, or primordial rocks of the solar system. However, impact-generated secondary features are abundant in chondrites, suggesting that collisions among early-formed planetesimals and their fragmentation and reassembly have been effective throughout the evolution of the solar system. In this report, we review evidence of the major role of impacts in generating the current mineralogical and petrographic characteristics of chondrites. We provide perspective to these meteoritic features by discussing recent analyses of large-scale structures of the main asteroid belt and remote-sensing observations of asteroids. Observations at various spatial scales all attest that the "primitive" materials formed during the evolution of the solar system have largely been reprocessed, confirming previous studies that primitivity is relative, not absolute. This implies that (1) chondrites (and some differentiated meteorites) should systematically be envisioned as reprocessed and heterogeneous materials and (2) brecciated meteorites should be considered the norm and unbrecciated meteorites the exception.

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Section: Meteoritic Evidence Of Widespread Collision Processes In the Asteroid Beltmentioning

confidence: 98%

The astrophysical context of collision processes in meteorites

Marrocchi

Delbò

Gounelle

2021

Meteorit & Planetary Scien

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“…The oxygen isotope composition of CM1s is similar to that of CM2s although they plot at the 16 O-rich end of the CM range suggesting that they were affected by the same water reservoir at a similar W/R ratio (Fig. 6), but their increased alteration may be due to higher temperatures of water interaction (King et al, 2018;Suttle et al, 2021;Vacher et al, 2019;Zolensky et al, 1997). In addition, the 16 O-rich composition could also partly reflect terrestrial alteration as all of these meteorites are finds (King et al, 2018).…”

Section: CMmentioning

confidence: 77%

“…The following studies were used in construction of this plot: For the CIs: Zolensky et al (1989Zolensky et al ( , 1993; Rowe et al (1994); Clayton and Mayeda (1999); Noguchi et al (2011). For the CM1s data from the recent review by Suttle et al (2021) and references therein and for Flensburg: Bischoff et al (2021). (Color figure can be viewed at wileyonlinelibrary.com.)…”

Section: Cymentioning

confidence: 99%

“…There is ample evidence that aqueous alteration in low petrologic type carbonaceous chondrite (CC) meteorites occurred mainly on their parent bodies (e.g., Brearley, 2006;Suttle et al, 2021), most likely predominantly through the melting of co-accreted ices (e.g., Matsumoto et al, 2019). Observations of the effects of the action of water on asteroids can provide quantitative constraints on their geological history (e.g., temperatures, water-to-rock [W/R] ratios, and fluid compositions) and can show how minerals interacted with co-accreting ices.…”

Section: Introductionmentioning

confidence: 99%

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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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“…Radiogenic dating of carbonate minerals associated with aqueous alteration in CM chondrites places their formation time between ~2.4 and 4 Myr after CAIs 43 . Based on alteration sequences proposed for CM chondrites, these minerals likely formed contemporaneously with pyrrhotite and magnetite 2,44 . Thus, it is unlikely that an endogenous magnetic field from a core dynamo magnetized the CM chondrites if model-predicted dynamo timing and the ages of the CM magnetized minerals are correct.…”

Section: Alternative Origins Of Magnetization In Planetesimalsmentioning

confidence: 99%

Magnetization of carbonaceous asteroids by nebular fields and the origin of CM chondrites

Courville

O’Rourke

Castillo‐Rogez

et al. 2021

Preprint

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The solar nebula carried a strong magnetic field that had a stable intensity and direction for periods of a thousand years or more 1 . The solar nebular field may have produced post-accretional magnetization in at least two groups of meteorites, CM and CV chondrites 1-3 , which originated from planetesimals that may have underwent aqueous alteration before gas in the solar nebula dissipated 1,3 . Magnetic minerals produced during aqueous alteration, such as magnetite and pyrrhotite 4 , could acquire a chemical remanent magnetization from that nebular field 3 . However, many questions about the size, composition, formation time, and, ultimately, identity of the parent bodies that produced magnetized CM and CV chondrites await answers-including whether a parent body might exhibit a detectable magnetic field today. Here, we use thermal evolution models to show that planetesimals that formed between a few Myr after CAIs and ~1 Myr before the nebular gas dissipated could acquire from the nebular field, and retain until today, a chemical remanent magnetization throughout nearly their entire volume. Hence, in-situ magnetometer measurements of C-type asteroids could help link magnetized asteroids to magnetized meteorites. Specifically, a future mission could search for a magnetic field as part of testing the hypothesis that 2 Pallas is the parent body of the CM chondrites 5 . Overall, large carbonaceous asteroids might record ancient magnetic fields in magnetic remanence that produces strong modern magnetic fields, even without a metallic core that once hosted a dynamo.

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The aqueous alteration of CM chondrites, a review

Cited by 55 publications

References 285 publications

The astrophysical context of collision processes in meteorites

The astrophysical context of collision processes in meteorites

Abundance and importance of petrological type 1 chondritic material

Magnetization of carbonaceous asteroids by nebular fields and the origin of CM chondrites

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