Oxygen Isotopes of Chondritic Components

Yurimoto, H.; Krot, Alexander N.; Choi, B. G.; Adnot, Jérôme; Kunihiro, T.; Brearley, A. J.

doi:10.2138/rmg.2008.68.8

Cited by 128 publications

(145 citation statements)

References 101 publications

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“…In-situ O isotope analyses have identified relict grains with CAI-like O isotope compositions inside chondrules (CAI stands for Ca-Al-rich inclusions, the first solids formed in the solar system). Thus, much of the spread in O isotope compositions among single chondrules may be related to the incorporation of 16 O-rich and CAI-like material into the 16 O-poor chondrule precursors Tenner et al 2017;Yurimoto et al 2008). Except for O, isotopic data of single chondrules are sparse, but recently Cr and Mg isotope data were reported for individual chondrules from CV, CR and CB chondrites (Olsen et al 2016;Van Kooten et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Mixing and Transport of Dust in the Early Solar Nebula as Inferred from Titanium Isotope Variations among Chondrules

Gerber

Burkhardt

Budde

et al. 2017

ApJL

102

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Chondrules formed by the melting of dust aggregates in the solar protoplanetary disk and as such provide unique insights into how solid material was transported and mixed within the disk. Here Ti variations can be attributed to the addition of isotopically heterogeneous CAI-like material to enstatite and ordinary chondrite-like chondrule precursors. The new Ti isotopic data demonstrate that isotopic variations among carbonaceous chondrite chondrules do not require formation over a wide range of orbital distances, but can instead be fully accounted for by the incorporation of isotopically anomalous 'nuggets' into chondrule precursors. As such, these data obviate the need for disk-wide transport of chondrules prior to chondrite parent body accretion and are consistent with formation of chondrules from a given chondrite group in localized regions of the disk. Lastly, the ubiquitous presence of 50 Ti-enriched material in carbonaceous chondrites, and the lack of this material in the non-carbonaceous chondrites support the idea that these two meteorite groups derive from areas of the disk that remained isolated from each other through the formation of Jupiter.

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Section: Introductionmentioning

confidence: 99%

Mixing and Transport of Dust in the Early Solar Nebula as Inferred from Titanium Isotope Variations among Chondrules

Gerber

Burkhardt

Budde

et al. 2017

ApJL

102

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“…Oxygen isotopes of chondrites, however, show evidence for heterogeneity between gas and solid. Oxygen isotopic compositions of CAIs and chondrules from carbonaceous chondrites are distributed along the CCAM line (Clayton et al 1983), which have been proved by later numerous analyses with secondary ionmicroprobe mass spectrometry (SIMS) (e.g., Yurimoto et al 2008 The oxygen abundance is measured relative to the abundance in the initial dust, and the value of about 5 corresponds to that of the average solar nebula. The isotope exchange efficiency is 1 and the cooling rate is 0.01.…”

Section: Discussionmentioning

confidence: 95%

The role of exchange reactions in oxygen isotope fractionation during CAI and chondrule formation

Nagahara¹,

Ozawa

2012

Meteorit & Planetary Scien

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Abstract-The role of oxygen isotope exchange during evaporation and condensation of silicate melt is quantitatively evaluated. Silicate dusts instantaneously heated above liquidus temperature are assumed to cool in gas and experience partial evaporation and subsequent recondensation. The results show that isotopic exchange effectively suppresses massdependent O-isotope fractionation even if the degree of evaporation is large, which is the fundamental difference from the case without isotopic exchange. The final composition of silicate melt strongly depends on the initial abundance of oxygen in the ambient gas relative to that in silicate dust, but not on the cooling rate of the system. The model was applied to O-isotope evolution of silicate melts in isotopically distinct gas of the protoplanetary disk. It was found that deviation from a straight mixing line toward the d18 O-rich side on the threeoxygen isotope diagram is inevitable when mass-dependent fractionation and isotopic exchange take place simultaneously; the degree of deviation depends on the abundance of oxygen in an ambient gas and isotopic exchange efficiency. The model is applied to explain O-isotopic compositions of igneous CAIs and chondrules.

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“…Isotopic compositions of water in carbonaceous chondrites are in the range of -500 to +100‰ for δD (Alexander et al, 2012) and -5 to +2‰ for ∆ 17 O (Yurimoto et al, 2008). The halite fluid inclusion brines plot outside the region of estimated carbonaceous chondrite water.…”

Section: Discussionmentioning

confidence: 95%

“…15 Alexander et al (2012); Clayton and Mayeda (1999); Clayton et al (1991); Hartogh et al (2011);McKeegan et al (2011);Sakamoto et al (2007);Yurimoto et al (2008) (McKeegan et al, 2011), Earth, Mars, achondrite (Ach), chondrite (Cht) (Clayton, 1993) (Yurimoto et al, 2008), cosmic symplectite (COS) (Sakamoto et al, 2007) …”

Section: Discussionmentioning

confidence: 99%

“…Oxygen isotopes in the solar system are also highly variable (Sakamoto et al, 2007;Yurimoto et al, 2008), reflecting contributions of an H 2 O component (Kuramoto and Yurimoto, 2005;Lyons and Young, 2005;Yurimoto and Kuramoto, 2004). However, it is impossible to measure isotopes of hydrogen and oxygen simultaneously in hydrous minerals, because they invariably contain structural oxygen not bound in water.…”

Section: A C Bmentioning

confidence: 99%

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Isotopic compositions of asteroidal liquid water trapped in fluid inclusions of chondrites

et al. 2014

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Determination of isotopic composition of extraterrestrial liquid water provides important information regarding the origin of water on Earth and the terrestrial planets. Fluid inclusions in halite of ordinary chondrites are the only direct samples of extraterrestrial liquid water available for laboratory measurements. We determined H and O isotopic compositions of this water by secondary ion mass spectrometry equipped with a cryogenic apparatus for sample cooling. Isotopic compositions of the fluid inclusion fluids (brines) were highly variable among individual inclusions, -400 < δD < +1300‰; -20 < ∆ 17 O < +30‰, indicating that these aqueous fluids were in isotopic disequilibrium before trapping in halite on asteroids. The isotopic variation of fluids shows that various degrees of water-rock interaction had been underway on the asteroids before trapping between D-rich-16 O-poor aqueous fluid, D-poor-16 O-rich aqueous fluid, and asteroidal rock by delivery of cometary water onto hydrous asteroids. This may be a fundamental mechanism in the evolution of modern planetary water.

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Oxygen Isotopes of Chondritic Components

Cited by 128 publications

References 101 publications

Mixing and Transport of Dust in the Early Solar Nebula as Inferred from Titanium Isotope Variations among Chondrules

Mixing and Transport of Dust in the Early Solar Nebula as Inferred from Titanium Isotope Variations among Chondrules

The role of exchange reactions in oxygen isotope fractionation during CAI and chondrule formation

Isotopic compositions of asteroidal liquid water trapped in fluid inclusions of chondrites

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