Calcium–aluminum‐rich inclusions in non‐carbonaceous chondrites: Abundances, sizes, and mineralogy

Dunham, E. T.; Sheikh, A.; Opara, D.; Matsuda, N.; Liu, M.‐C.; McKeegan, K. D.

doi:10.1111/maps.13975

Cited by 7 publications

(1 citation statement)

References 93 publications

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“…The numbers are overall consistent with those from the previous study using Ni- and CI-normalized HSE abundances ( 44 ). The high CAI abundance for the IVB precursor materials has been observed in a few asteroids ( 63 ), and some CV and CK chondrites have been found to have high CAI abundances of 16% by area ( 64 ), approaching the values that we model for the groups IID and IIIF. Additionally, the paucity of high-CAI asteroids and chondrites could be attributable to the heating and melting of large CAI-rich bodies due to the decay of 26 Al (t½ = 717,000 y).…”

Section: Discussionsupporting

confidence: 66%

Compositions of iron-meteorite parent bodies constrain the structure of the protoplanetary disk

Zhang,

Chabot,

Rubin

2024

Proc. Natl. Acad. Sci. U.S.A.

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Magmatic iron-meteorite parent bodies are the earliest planetesimals in the Solar System, and they preserve information about conditions and planet-forming processes in the solar nebula. In this study, we include comprehensive elemental compositions and fractional-crystallization modeling for iron meteorites from the cores of five differentiated asteroids from the inner Solar System. Together with previous results of metallic cores from the outer Solar System, we conclude that asteroidal cores from the outer Solar System have smaller sizes, elevated siderophile-element abundances, and simpler crystallization processes than those from the inner Solar System. These differences are related to the formation locations of the parent asteroids because the solar protoplanetary disk varied in redox conditions, elemental distributions, and dynamics at different heliocentric distances. Using highly siderophile-element data from iron meteorites, we reconstruct the distribution of calcium-aluminum-rich inclusions (CAIs) across the protoplanetary disk within the first million years of Solar-System history. CAIs, the first solids to condense in the Solar System, formed close to the Sun. They were, however, concentrated within the outer disk and depleted within the inner disk. Future models of the structure and evolution of the protoplanetary disk should account for this distribution pattern of CAIs.

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Section: Discussionsupporting

confidence: 66%

Compositions of iron-meteorite parent bodies constrain the structure of the protoplanetary disk

Zhang,

Chabot,

Rubin

2024

Proc. Natl. Acad. Sci. U.S.A.

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Chondrule Properties and Formation Conditions

Marrocchi,

Jones,

Russell

et al. 2024

Space Sci Rev

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Chondrules are iconic sub-millimeter spheroids representing the most abundant high-temperature dust formed during the evolution of the circumsolar disk. Chondrules have been the subject of a great deal of research, but no consensus has yet emerged as to their formation conditions. In particular, the question of whether chondrules are of nebular or planetary origin remains largely debated. Building upon decades of chondrule investigation and recent headways in combining petrographic observations and O−Ti−Cr isotopic compositions, we here propose a comprehensive vision of chondrule formation. This holistic approach points toward a nebular origin of both NC and CC chondrules, with repetitive high-temperature recycling processes controlling the petrographic and isotopic diversities shown by chondrules. Chondrule precursors correspond to mixing between (i) early-formed refractory inclusions ± NC-like dust and (ii) previous generation of chondrules ± CI-like material. Chondrule formation took place under open conditions with gas-melt interactions with multi-species gas (H2O, Mg, SiO) playing a key role for establishing their characteristics. Petrographic and isotopic systematics do not support disk-wide transport of chondrules but point toward local formation of chondrules within their respective accretion reservoirs. Altogether, this shows that several generations of genetically-related chondrules (i.e., deriving from each other) co-exist in chondrites. In addition to supporting the nebular brand of chondrule-forming scenarios, this argues for repetitive and extremely localized heating events for producing chondrules.

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Is There a Genetic Relationship Between Chondrules and Matrix?

van Kooten,

Brearley,

Ebel

et al. 2024

Space Sci Rev

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Chondritic components such as chondrules and matrix are the key time capsules that can help us understand the evolution and dynamics of the protoplanetary disk from which the Solar System originated. Knowledge of where and how these components formed and to what extent they were transported in the gaseous disk provides major constraints to astrophysical models that investigate planet formation. Here, we explore whether chondrules and matrix are genetically related to each other and formed from single reservoirs per chondrite group or if every chondrite represents a unique proportion of components transported from a small number of formation reservoirs in the disk. These ‘static versus dynamic disk’ interpretations of cosmochemical data have profound implications for the accretion history of the planets in the Solar System. To fully understand the relationship between chondrules and matrix and their potential “complementarity”, we dive into the petrological nature and origin of matrix, the chemical and isotopic compositions of chondrules and matrix and evaluate these data considering the effect of secondary alteration observed in chondrites and the potential complexity of chondrule formation. Even though we, the authors, have used different datasets and arrived at differing interpretations of chondrule-matrix relationships in the past, this review provides clarity on the existing data and has given us new directions towards future research that can resolve the complementarity debate.

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Calcium–aluminum‐rich inclusions in non‐carbonaceous chondrites: Abundances, sizes, and mineralogy

Cited by 7 publications

References 93 publications

Compositions of iron-meteorite parent bodies constrain the structure of the protoplanetary disk

Compositions of iron-meteorite parent bodies constrain the structure of the protoplanetary disk

Chondrule Properties and Formation Conditions

Is There a Genetic Relationship Between Chondrules and Matrix?

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