Molybdenum isotopic evidence for the origin of chondrules and a distinct genetic heritage of carbonaceous and non-carbonaceous meteorites

Budde, G.; Burkhardt, C.; Brennecka, G. A.; Fischer-Gödde, M.; Kruijer, T. S.; Kleine, T.

doi:10.1016/j.epsl.2016.09.020

Cited by 228 publications

(229 citation statements)

References 49 publications

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“…After digestion of the iron meteorites in concentrated HNO 3 -HCl (2:1), the sample solutions were split into a fraction for W and Mo (∼90%) and for Pt (∼10%) isotope analysis. The chemical separation of W, Pt, and Mo was accomplished using ion exchange chromatography following previously published procedures (6,12,15,36 …”

Section: Methodsmentioning

confidence: 99%

“…implies that by this time, the NC and CC reservoirs were already separated. The distinction between the NC and CC reservoirs most likely reflects the addition of presolar material enriched in r-process nuclides to the solar nebula region from which the CC meteorites derive (12). Given that all CC meteorites plot on a single s-process mixing line with a constant offset compared with the NC line ( Fig.…”

Section: Coexistence and Spatial Separation Of CC And Nc Meteorite Rementioning

confidence: 99%

“…For instance, Cr, Ti, and Mo isotope anomalies (6)(7)(8)12) reveal a fundamental dichotomy in the genetic heritage of meteorites, distinguishing between "noncarbonaceous" and "carbonaceous" meteorite reservoirs (11). This distinction may reflect either a temporal change in disk composition or the separation of materials accreted inside [noncarbonaceous (NC) meteorites] and outside [carbonaceous (CC) meteorites] the orbit of Jupiter (11)(12)(13)(14). If the latter is correct, then the age of Jupiter can be determined by assessing the formation time and longevity of the NC and CC meteorite reservoirs.…”

mentioning

confidence: 99%

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Age of Jupiter inferred from the distinct genetics and formation times of meteorites

Kruijer

Burkhardt

Budde

et al. 2017

Proc. Natl. Acad. Sci. U.S.A.

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586

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Significance Jupiter is the most massive planet of the Solar System and its presence had an immense effect on the dynamics of the solar accretion disk. Knowing the age of Jupiter, therefore, is key for understanding how the Solar System evolved toward its present-day architecture. However, although models predict that Jupiter formed relatively early, until now, its formation has never been dated. Here we show through isotope analyses of meteorites that Jupiter’s solid core formed within only ∼1 My after the start of Solar System history, making it the oldest planet. Through its rapid formation, Jupiter acted as an effective barrier against inward transport of material across the disk, potentially explaining why our Solar System lacks any super-Earths.

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Section: Methodsmentioning

confidence: 99%

Section: Coexistence and Spatial Separation Of CC And Nc Meteorite Rementioning

confidence: 99%

mentioning

confidence: 99%

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Age of Jupiter inferred from the distinct genetics and formation times of meteorites

Kruijer

Burkhardt

Budde

et al. 2017

Proc. Natl. Acad. Sci. U.S.A.

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515

586

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“…The origin of these once-molten silicate spherules remains debated, but the currently favored hypothesis states that chondrules formed by the melting of dust aggregates in the solar nebula, induced by shock waves or current sheets (e.g., Desch et al 2005;McNally et al 2013;Morris et al 2012). Alternative models, such as those in which chondrules are the result of protoplanetary impacts (e.g., Sanders & Scott 2012), are problematic because they cannot satisfy the chemical (Bland et al 2005;Ebel et al 2016;Hezel & Palme 2008;Palme et al 2015) and isotopic (Budde et al 2016a;Budde et al 2016b) complementarity observed between chondrules and matrix. This complementarity implies that within a given chondrite, chondrules and matrix derive from a common reservoir of dust, and that after their formation neither appreciable chondrules nor matrix were lost.…”

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

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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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“…Carbonaceous chondrites are fragments of hydrated asteroids that likely represent left-over building blocks of the outer Solar System, beyond the accretion region of Jupiter (Van Kooten et al, 2016;Olsen et al, 2016;Budde et al, 2016). These meteorites are among the oldest and most primitive objects that provide insights into the early protoplanetary disk and the formation and dynamics of the planets (Scott, 2007).…”

Section: Introductionmentioning

confidence: 99%

Isotope record of mineralogical changes in a spectrum of aqueously altered CM chondrites

Kooten

Nagashima

Kasama

et al. 2018

Geochimica et Cosmochimica Acta

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The recent fall of the relatively unaltered CM chondrite Maribo provides a unique opportunity to study the early stages of aqueous alteration on the CM chondrite parent body. We show using transmission electron microscopy of a matrix FIBsection from Maribo that this meteorite mainly appears to consist of tochilinite-cronstedtite intergrowths (TCIs), but also contains regions of amorphous or nanocrystalline silicates, anhydrous silicates and FeNi metal aggregates with thin iron oxide rims, suggesting that it experienced aqueous alteration to a relatively small degree. A comparison of Maribo with increasingly altered CM chondrites such as Jbilet Winselwan and Bells shows that during progressive aqueous alteration (1) the TCIs are replaced by coarser sulfides and increasingly Mg-rich serpentine, and (2) the abundance of 15 N-rich hotspots increases, whereas the magnitude of their 15 N enrichment decreases. We observe that the overall N isotope variability related to aqueous alteration is an order of magnitude lower than the variability observed between different chondrite groups. We suggest these high order differences are the result of heterogeneous accretion of insoluble or soluble organic carriers of 15 N to the different chondrite parent bodies. D/H ratios of matrices from Maribo, Jbilet Winselwan and Bells increase with progressive aqueous alteration, a trend that is opposite to expectations of mixing between D-poor water and D-rich organic matter. We argue that this behaviour cannot be related to Fe oxidation or serpentinization reactions and subsequent loss of D-poor H 2 gas. We offer an alternative hypothesis and suggest that CM chondrites experienced two-stage aqueous alteration. During the first stage occurring at relatively low temperature, mixing of increasing amounts of D-poor water with D-rich organic matter results in a decrease of D/H ratio with increasing degree of alteration. During the second stage of alteration occurring at relatively high temperature (T < 300°C), decomposition of TCIs in CMs of petrologic type <2.7 releases gaseous D-poor water that results in increase of the D/H ratio of the CM matrices. Finally, we report on changes in the organic structure of Maribo, Jbilet Winselwan and Bells using Carbon-K and Nitrogen-K edge electron energy loss spectroscopy. The organic matter initially has higher aromatic/aliphatic ratios (e.g., Maribo) and lower abundances of ketone and carboxyl functional groups, which we suggest are the result of chemical degradation of double bonded carbon from oxidation during hydrothermal

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Molybdenum isotopic evidence for the origin of chondrules and a distinct genetic heritage of carbonaceous and non-carbonaceous meteorites

Cited by 228 publications

References 49 publications

Age of Jupiter inferred from the distinct genetics and formation times of meteorites

Age of Jupiter inferred from the distinct genetics and formation times of meteorites

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

Isotope record of mineralogical changes in a spectrum of aqueously altered CM chondrites

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