Variations in the O-isotope composition of gas during the formation of chondrules from the CR chondrites

Devin Schrader, Kazuhide Nagashima, Alexander N. Krot, Ryan C. Ogliore, Eric Hellebrand

Research output: Contribution to journalArticle

22 Citations (Scopus)

Abstract

To better understand the environment of chondrule formation and constrain the O-isotope composition of the ambient gas in the Renazzo-like carbonaceous (CR) chondrite chondrule-forming region, we studied the mineralogy, petrology, and in situ O-isotope compositions of olivine in 11 barred olivine (BO) chondrules and pyroxene and silica in three type I porphyritic chondrules from the CR chondrites Gao-Guenie (b), Graves Nunataks (GRA) 95229, Pecora Escarpment (PCA) 91082, and Shişr 033. BO chondrules experienced a higher degree of melting than porphyritic chondrules, and therefore, it has been hypothesized that they more accurately recorded the O-isotope composition of the gas in chondrule-forming regions. We studied the O-isotope composition of silica as it has been hypothesized to have formed via direct condensation from the gas.BO chondrules constitute ~4% of the total CR chondrule population by volume. On a three-isotope oxygen diagram (δ17O vs. δ18O), olivine phenocrysts in type I and type II BO chondrules plot along ~slope-1 line; with the exception of a type II BO chondrule that plots along ~slope-0.5 line. Olivine phenocrysts in type I and type II BO chondrules have similar but more restricted ranges of δ17O values (~-3.8‰ to ~-1.3‰ and ~-0.8‰ to ~+1.4‰, respectively) than those in type I and type II porphyritic chondrules (~-4.6‰ to ~-0.3‰ and ~-1.8‰ to ~+0.9‰, respectively). The observation that olivine grains in type I BO chondrules have similar chemical and O-isotope compositions to those of olivine in their porphyritic counterparts argues against the hypothesis that olivine grains in type I porphyritic chondrules are xenocrysts and represent relict fragments of early formed planetesimals.The compositional and O-isotope data suggest that BO chondrules experienced more extensive, but incomplete exchange with the ambient gas than porphyritic chondrules. We suggest that CR chondrules formed from relatively 16O-enriched solids in the presence of relatively 16O-depleted gaseous H2O. The O-isotope compositions of chondrule olivine likely result from differences in the O-isotope composition of both the chondrule precursors and the ambient gas during chondrule formation. The inferred O-isotope composition of this gas (δ17O ranges from ~-3‰ to +3‰) is inconsistent with a high abundance of water from the outer Solar System, which has been predicted to be isotopically heavy.

Original languageEnglish (US)
Pages (from-to)50-74
Number of pages25
JournalGeochimica et Cosmochimica Acta
Volume132
DOIs
StatePublished - May 1 2014
Externally publishedYes

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chondrule
carbonaceous chondrite
Isotopes
Gases
isotope
olivine
Chemical analysis
gas
Silicon Dioxide
Oxygen Isotopes
Petrology
Mineralogy
Solar system
silica

ASJC Scopus subject areas

  • Geochemistry and Petrology

Cite this

Variations in the O-isotope composition of gas during the formation of chondrules from the CR chondrites. / Schrader, Devin; Nagashima, Kazuhide; Krot, Alexander N.; Ogliore, Ryan C.; Hellebrand, Eric.

In: Geochimica et Cosmochimica Acta, Vol. 132, 01.05.2014, p. 50-74.

Research output: Contribution to journalArticle

Schrader, Devin ; Nagashima, Kazuhide ; Krot, Alexander N. ; Ogliore, Ryan C. ; Hellebrand, Eric. / Variations in the O-isotope composition of gas during the formation of chondrules from the CR chondrites. In: Geochimica et Cosmochimica Acta. 2014 ; Vol. 132. pp. 50-74.
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N2 - To better understand the environment of chondrule formation and constrain the O-isotope composition of the ambient gas in the Renazzo-like carbonaceous (CR) chondrite chondrule-forming region, we studied the mineralogy, petrology, and in situ O-isotope compositions of olivine in 11 barred olivine (BO) chondrules and pyroxene and silica in three type I porphyritic chondrules from the CR chondrites Gao-Guenie (b), Graves Nunataks (GRA) 95229, Pecora Escarpment (PCA) 91082, and Shişr 033. BO chondrules experienced a higher degree of melting than porphyritic chondrules, and therefore, it has been hypothesized that they more accurately recorded the O-isotope composition of the gas in chondrule-forming regions. We studied the O-isotope composition of silica as it has been hypothesized to have formed via direct condensation from the gas.BO chondrules constitute ~4% of the total CR chondrule population by volume. On a three-isotope oxygen diagram (δ17O vs. δ18O), olivine phenocrysts in type I and type II BO chondrules plot along ~slope-1 line; with the exception of a type II BO chondrule that plots along ~slope-0.5 line. Olivine phenocrysts in type I and type II BO chondrules have similar but more restricted ranges of δ17O values (~-3.8‰ to ~-1.3‰ and ~-0.8‰ to ~+1.4‰, respectively) than those in type I and type II porphyritic chondrules (~-4.6‰ to ~-0.3‰ and ~-1.8‰ to ~+0.9‰, respectively). The observation that olivine grains in type I BO chondrules have similar chemical and O-isotope compositions to those of olivine in their porphyritic counterparts argues against the hypothesis that olivine grains in type I porphyritic chondrules are xenocrysts and represent relict fragments of early formed planetesimals.The compositional and O-isotope data suggest that BO chondrules experienced more extensive, but incomplete exchange with the ambient gas than porphyritic chondrules. We suggest that CR chondrules formed from relatively 16O-enriched solids in the presence of relatively 16O-depleted gaseous H2O. The O-isotope compositions of chondrule olivine likely result from differences in the O-isotope composition of both the chondrule precursors and the ambient gas during chondrule formation. The inferred O-isotope composition of this gas (δ17O ranges from ~-3‰ to +3‰) is inconsistent with a high abundance of water from the outer Solar System, which has been predicted to be isotopically heavy.

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