A link between oxygen, calcium and titanium isotopes in 26Al-poor hibonite-rich CAIs from Murchison and implications for the heterogeneity of dust reservoirs in the solar nebula

Kööp, L.; Davis, A. M.; Nakashima, D.; Park, Changkun; Krot, Alexander N.; Nagashima, K.; Tenner, T. J.; Heck, Philipp R.; Kita, N. T.

doi:10.1016/j.gca.2016.05.014

Cited by 94 publications

(91 citation statements)

References 67 publications

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“…Thus, the refractory CAI-like material added to the precursors of CV chondrules must have been heterogeneous for ε 50 Ti, with values that most likely ranged from the large excesses observed for CAIs to significantly lower values, perhaps as low as measured for EC-and OC-like material. It is noteworthy that hibonite grains from carbonaceous chondrites display large variations in 50 Ti (e.g., Fahey et al 1987;Ireland 1988;Kööp et al 2016), and as such might have contributed to the 50 Ti heterogeneity observed for the CAI-like material. However, in contrast to the Ti isotope anomalies observed at the bulk chondrite and individual chondrule scale, the 50 Ti variations in hibonites are not correlated with anomalies in 46 Ti.…”

Section: Samples and Methodsmentioning

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: Samples and Methodsmentioning

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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“…, ; Kööp et al. 2016a; Park et al. ), whereas others are isotopically more normal (e.g., Kööp et al.…”

Section: Multiple Generations Of Refractory Inclusions and Mechanismsmentioning

confidence: 99%

“…(1) The former are often isotopically anomalous compared to the isotopically more normal 26 Al‐rich CAIs (e.g., Ireland ; Sahijpal and Goswami ; Kööp et al. 2016a, 2016b). (2) The inferred ( 26 Al/ 27 Al) 0 ratios in many 26 Al‐poor CAIs are less than the 26 Al/ 27 Al ratios in the host meteorites required to explain thermal histories of their parent asteroids (e.g., Sugiura and Fujiya ; Doyle et al.…”

Section: Origin and Distribution Of 26al In The Ppdmentioning

confidence: 99%

“…2019a, 2019b), the 26 Al‐rich spinel‐hibonite inclusions, and in the platy hibonite crystals (PLACs) with ( 26 Al/ 27 Al) 0 typically <5 × 10 –6 from CM chondrites (Kööp et al. 2016a, 2016b) and grossite‐bearing CAIs from CH chondrites (Gounelle et al. ; Krot et al.…”

Section: Oxygen Isotopic Compositions Of Chondrites and Their Componentsmentioning

confidence: 99%

“…For example, it does not explain the apparent correlation of Δ 17 O with magnitude of isotope anomalies in CM PLACs (Kööp et al. 2016a). In addition, this process must be very efficient, because amorphous silicates with solar‐like Δ 17 O in meteorites or cometary dust have not been discovered yet.…”

Section: Oxygen Isotopic Compositions Of Chondrites and Their Componentsmentioning

confidence: 99%

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Refractory inclusions in carbonaceous chondrites: Records of early solar system processes

Krot

2019

Meteorit & Planetary Scien

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Chondrites consist of three major components: refractory inclusions (Ca,Al‐rich inclusions [CAIs] and amoeboid olivine aggregates), chondrules, and matrix. Here, I summarize recent results on the mineralogy, petrology, oxygen, and aluminum‐magnesium isotope systematics of the chondritic components (mainly CAIs in carbonaceous chondrites) and their significance for understanding processes in the protoplanetary disk (PPD) and on chondrite parent asteroids. CAIs are the oldest solids originated in the solar system: their U‐corrected Pb‐Pb absolute age of 4567.3 ± 0.16 Ma is considered to represent time 0 of its evolution. CAIs formed by evaporation, condensation, and aggregation in a gas of approximately solar composition in a hot (ambient temperature >1300 K) disk region exposed to irradiation by solar energetic particles, probably near the protoSun; subsequently, some CAIs were melted in and outside their formation region during transient heating events of still unknown nature. In unmetamorphosed, type 2–3.0 chondrites, CAIs show large variations in the initial 26Al/27Al ratios, from <5 × 10–6 to ~5.25 × 10–5. These variations and the inferred low initial abundance of 60Fe in the PPD suggest late injection of 26Al by a wind from a nearby Wolf–Rayet star into the protosolar molecular cloud core prior to or during its collapse. Although there are multiple generations of CAIs characterized by distinct mineralogies, textures, and isotopic (O, Mg, Ca, Ti, Mo, etc.) compositions, the 26Al heterogeneity in the CAI‐forming region(s) precludes determining the duration of CAIs formation using 26Al‐26Mg systematics. The existence of multiple generations of CAIs and the observed differences in CAI abundances in carbonaceous and noncarbonaceous chondrites may indicate that CAIs were episodically formed and ejected by a disk wind from near the Sun to the outer solar system and then spiraled inward due to gas drag. In type 2–3.0 chondrites, most CAIs surrounded by Wark–Lovering rims have uniform Δ17O (= δ17O−0.52 × δ18O) of ~ −24‰; however, there is a large range of Δ17O (from ~−40 to ~ −5‰) among them, suggesting the coexistence of 16O‐rich (low Δ17O) and 16O‐poor (high Δ17O) gaseous reservoirs at the earliest stages of the PPD evolution. The observed variations in Δ17O of CAIs may be explained if three major O‐bearing species in the solar system (CO, H2O, and silicate dust) had different O‐isotope compositions, with H2O and possibly silicate dust being 16O‐depleted relative to both the Genesis solar wind Δ17O of −28.4 ± 3.6‰ and even more 16O‐enriched CO. Oxygen isotopic compositions of CO and H2O could have resulted from CO self‐shielding in the protosolar molecular cloud (PMC) and the outer PPD. The nature of 16O‐depleted dust at the earliest stages of PPD evolution remains unclear: it could have either been inherited from the PMC or the initially 16O‐rich (solar‐like) MC dust experienced O‐isotope exchange during thermal processing in the PPD. To understand the chemical and isotopic composition of the protosolar MC...

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Titanium isotopic fractionation during magmatic differentiation

Zhao

Tang

et al. 2020

Contrib Mineral Petrol

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A link between oxygen, calcium and titanium isotopes in 26Al-poor hibonite-rich CAIs from Murchison and implications for the heterogeneity of dust reservoirs in the solar nebula

Cited by 94 publications

References 67 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

Refractory inclusions in carbonaceous chondrites: Records of early solar system processes

Titanium isotopic fractionation during magmatic differentiation

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