Volume 60, Issue 4 pp. 717-743
Article

Type B–type C CAI in a CR chondrite: Evidence for multiple melting events, gas–melt interaction, and oxygen-isotope exchange

Kirsten Larsen

Kirsten Larsen

Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark

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Alexander N. Krot

Corresponding Author

Alexander N. Krot

Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark

Hawaii Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, Hawaii, USA

Correspondence

Alexander N. Krot, Centre for Star and Planet Formation, University of Copenhagen, Copenhagen DK-1350, Denmark.

Email: [email protected]

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Daniel Wielandt

Daniel Wielandt

Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark

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Kazuhide Nagashima

Kazuhide Nagashima

Hawaii Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, Hawaii, USA

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Guy Libourel

Guy Libourel

Observatoire de la Côte d'Azur, UMR 7293 LAGRANGE, Nice, France

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Martin Bizzarro

Martin Bizzarro

Centre for Star and Planet Formation, University of Copenhagen, Copenhagen, Denmark

Hawaii Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, Honolulu, Hawaii, USA

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First published: 20 March 2025

Editorial Handling—Marrocchi Yves

Abstract

A coarse-grained igneous calcium-aluminum-rich inclusion (CAI) N-53, 4.3 × 5.9 mm in size, from the CR (Renazzo-type) carbonaceous chondrite Northwest Africa (NWA) 6043 is composed of two mineralogically, chemically, and isotopically distinct units—type B (B) and type C (C). Type B unit occurs in the CAI core and consists of melilite (Åk28–56), AlTi-diopside, anorthite, spinel, and minor Fe,Ni-metal. Type C unit forms islands in B (Cc) and mantle (Cm) around it and consists of Na-bearing åkermanitic melilite (Åk58–72, 0.18–0.86 wt% Na2O), anorthite, AlTi-diopside (up to 1.2 wt% Cr2O3), spinel (up to 2.1 wt% Cr2O3), perovskite, and minor wollastonite. The outermost portion of N-53 contains relict grains of olivine (Fa4) and low-Ca pyroxene (Fs4Wo5); Wark–Lovering rim is absent. Magnesian spinel in B and C is 16O-rich (Δ17O ~ −23‰); Cr-bearing spinel in Cm is 16O-depleted (Δ17O ~ −11‰). AlTi-diopside, anorthite, and melilite in B and Cc are 16O-depleted to various degrees (Δ17O ~ −22‰ to −19‰, −21‰ to −17‰, −13‰ to −8‰, respectively). AlTi-diopside, anorthite, and melilite in Cm show a range of compositions correlated with a distance from the CAI edge (Δ17O ~ −18‰ to −8‰, −16‰ to −8‰, ~ −8‰ to −2‰). Melilite in B has the heaviest Mg-isotope composition (Δ25Mg ~ 10‰); average Δ25Mg of melilite, AlTi-diopside, and spinel in C are ~9, ~8‰, and ~6‰, respectively; anorthite in both units has Δ25Mg of ~4‰. On the Al-Mg evolutionary diagram, melilite data in B oscillate around the canonical isochron. Melilite, AlTi-diopside, and spinel in C have resolvable δ26Mg* and deviate to the left of this isochron; anorthite in both units has barely resolvable δ26Mg*. Although these data are consistent with late-stage reprocessing of N-53, they provide no clear chronological information. We conclude that N-53 experienced multiple melting events. Initial melting of solid precursors took place in an 16O-rich gaseous reservoir and resulted in formation of the uniformly 16O-rich (Δ17O ~ −24‰) type B CAI. Subsequent single- or multi-stage partial melting of this CAI occurred in an 16O-depleted gaseous reservoir(s) and resulted in addition of SiO and Na to the CAI melt, O- and Mg-isotope exchange, and crystallization of C unit.

Data Availability Statement

The data that support the findings of this study are available on request from the corresponding author. The data are not publicly available due to privacy or ethical restrictions.

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