26 Al– 26 Mg systematics in chondrules from Kaba and Yamato 980145 CV3 carbonaceous chondrites

Nagashima, K.; Krot, Alexander N.; Komatsu, M.

doi:10.1016/j.gca.2016.10.030

Cited by 49 publications

(30 citation statements)

References 82 publications

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“…1). The CR chondrules seem to have formed later, at ~3.7 Ma after CAI formation (Amelin et al 2002;Schrader et al 2017), than CV chondrules at ~2.2 Ma after CAI formation (Budde et al 2016b;Luu et al 2015;Nagashima et al 2017). Therefore, one explanation for the smaller 50 Ti heterogeneity among CR compared to CV chondrules is an increasing homogenization of the added 50 Ti-enriched CAI-like material over time.…”

Section: Samples and Methodsmentioning

confidence: 99%

“…Further, the two meteorite reservoirs must have remained separated for at least ~2-3 Ma, because they both contain chondrites, which accreted between ~2 and ~4 Ma after CAI formation (Budde et al 2016a;Luu et al 2015;Nagashima et al 2017;Schrader et al 2017;Ushikubo et al 2013). Thus, the dust carriers of the supernova-derived material that had been added to the carbonaceous meteorite reservoir did not infiltrate the reservoir of the non-carbonaceous meteorites for at least 2-3 Ma (Budde et al 2016a).…”

Section: Separation Of Carbonaceous and Non-carbonaceous Meteorite Rementioning

confidence: 99%

See 1 more Smart Citation

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%

Section: Separation Of Carbonaceous and Non-carbonaceous Meteorite Rementioning

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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“…; Nagashima et al. ); therefore, differentiation of these rapidly accreted chondrite parent bodies is unlikely. These observations do not preclude accretion of chondritic materials on the earlier formed and possibly differentiated bodies—a hypothesis recently proposed to explain paleomagnetic records of CV3 chondrites (Elkins‐Tanton et al.…”

Section: Origin and Distribution Of 26al In The Ppdmentioning

confidence: 99%

“…Model calculations show that the initial abundance of 26 Al in chondrules can explain peak metamorphic temperatures reached by their host meteorites (e.g., Sugiura and Fujiya 2014), suggesting rapid accretion of chondrules after their formation into their host asteroids (Alexander et al 2008). At the same time, the abundance of 26 Al in chondrules is not enough to melt asteroids (Kunihiro et al 2004;Nagashima et al 2017); therefore, differentiation of these rapidly accreted chondrite parent bodies is unlikely. These observations do not preclude accretion of chondritic materials on the earlier formed and possibly differentiated bodies-a hypothesis recently proposed to explain paleomagnetic records of CV3 chondrites (Elkins-Tanton et al 2011;Gattacceca et al 2016).…”

Section: Al-mg Isotope Systematics In Chondrules: Thermal Evolution Omentioning

confidence: 99%

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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“…Al‐Mg formation ages of CV 3 chondrules (~2.0–3.4 Ma after CAI formation; Mishra and Chaussidon ; Nagashima et al. ) and Mn‐Cr ages of fayalite and Ca,Fe‐silicates (~3.2–4.2 Ma after CAI formation; Doyle et al. ; Jogo et al.…”

Section: Resultsmentioning

confidence: 99%

Origin of the metamorphosed clasts in the CV3 carbonaceous chondrite breccias of Graves Nunataks 06101, Vigarano, Roberts Massif 04143, and Yamato‐86009

Jogo

Ito

Wakita

et al. 2019

Meteorit & Planetary Scien

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We observed metamorphosed clasts in the CV3 chondrite breccias Graves Nunataks 06101, Vigarano, Roberts Massif 04143, and Yamato-86009. These clasts are coarse-grained polymineralic rocks composed of Ca-bearing ferroan olivine (Fa 24-40 , up to 0.6 wt% CaO), diopside (Fs 7-12 Wo 44-50 ), plagioclase (An 52-75 ), Cr-spinel (Cr/[Cr + Al] = 0.4, Fe/[Fe + Mg] = 0.7), sulfide and rare grains of Fe-Ni metal, phosphate, and Ca-poor pyroxene (Fs 24 Wo 4 ). Most clasts have triple junctions between silicate grains. The rare earth element (REE) abundances are high in diopside (REE~3.80-13.83 9 CI) and plagioclase (Eu~12.31-14.67 9 CI) but are low in olivine (REE~0.01-1.44 9 CI) and spinel (REẼ 0.25-0.49 9 CI). These REE abundances are different from those of metamorphosed chondrites, primitive achondrites, and achondrites, suggesting that the clasts are not fragments of these meteorites. Similar mineralogical characteristics of the clasts with those in the Mokoia and Yamato-86009 breccias (Jogo et al. 2012) suggest that the clasts observed in this study would also form inside the CV3 chondrite parent body. Thermal modeling suggests that in order to reach the metamorphosed temperatures of the clasts of >800°C, the clast parent body should have accreted by~2.5-2.6 Ma after CAIs formation. The consistency of the accretion age of the clast parent body and the CV3 chondrule formation age suggests that the clasts and CV3 chondrites could be originated from the same parent body with a peak temperature of 800-1100°C. If the body has a peak temperature of >1100°C, the accretion age of the body becomes older than the CV3 chondrule formation age and multiple CV3 parent bodies are likely.

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26 Al– 26 Mg systematics in chondrules from Kaba and Yamato 980145 CV3 carbonaceous chondrites

Cited by 49 publications

References 82 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

Origin of the metamorphosed clasts in the CV3 carbonaceous chondrite breccias of Graves Nunataks 06101, Vigarano, Roberts Massif 04143, and Yamato‐86009

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