Origin of the non-carbonaceous–carbonaceous meteorite dichotomy

Nanne, J. A. M.; Nimmo, F.; Cuzzi, Jeffrey N.; Kleine, T.

doi:10.1016/j.epsl.2019.01.027

Cited by 154 publications

(191 citation statements)

References 48 publications

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“…1a), this indicates that the injection function of r-process contributions decreased during infall. This has also been suggested by Nanne et al (2019); Burkhardt et al (2019). So we may think of the x (increasing with time) plotted in the paper to represent the complement of the r-process component, if these runs are to be likened to the forming solar system.…”

Section: Refractory Inclusions As Probes Of the Infall Stagementioning

confidence: 69%

“…We see that, on the whole, x decreases with heliocentric distance, indicating that the earliest isotopic signatures dominate in the outer disk, despite their having been originally injected in the inner disk (as it had lower specific angular momentum). This is because the viscous expansion of the disk efficiently advected early material outward (see also Nanne et al (2019)) and the non-transported material has been rapidly accreted by the protoSun. There is nonetheless a slight increase discernible just inside the final centrifugal radius (11 AU) where most of the latest (high-x) material has been injected, but this washes out during the subsequent "closed-system" evolution of the star+disk system.…”

Section: Resultsmentioning

confidence: 99%

“…In principle, one could evade the contradiction by denying the inversion of the parental cloud gradient (Visser et al 2009;Nanne et al 2019). This could come about for a greater centrifugal radius, as in our faster rotator runs (which would however greatly diminish the abundance of refractory inclusions; see Fig.…”

Section: The Carbonaceous/non-carbonaceous Chondrite Dichotomymentioning

confidence: 92%

“…had spatially varying proportions of the different presolar grain populations), and, as it sequentially collapsed to form the solar protoplanetary disk, passed on some of this heterogeneity to it, before turbulent mixing gradually reduced its extent (e.g. Huss & Lewis 1995;Dauphas & Schauble 2016;Nanne et al 2019). In fact, the CAI formation epoch duration appears commensurate with infall timescales (Yang & Ciesla 2012;Pignatale et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Jacquet

Pignatale

Chaussidon

et al. 2019

ApJ

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The isotopic heterogeneity of the Solar System shown by meteorite analyses is more pronounced for its earliest objects, the Calcium-Aluminum-rich Inclusions (CAIs). This suggests that it was inherited from spatial variations in different stardust populations in the protosolar cloud. We model the formation of the solar protoplanetary disk following its collapse and find that the solid-weighted standard deviation of different nucleosynthetic contributions in the disk is reduced by one order of magnitude compared to the protosolar cloud, whose successive isotopic signatures are fossilized by CAIs. The enrichment of carbonaceous chondrites in r-process components, whose proportions are inferred to have diminished near the end of infall, is consistent with their formation at large heliocentric distances, where the early signatures would have been preferentially preserved after outward advection. We also argue that thermal processing had little effect on the (mass-independent) isotopic composition of bulk meteorites for refractory elements.

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Section: Refractory Inclusions As Probes Of the Infall Stagementioning

confidence: 69%

Section: Resultsmentioning

confidence: 99%

Section: The Carbonaceous/non-carbonaceous Chondrite Dichotomymentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

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Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Jacquet

Pignatale

Chaussidon

et al. 2019

ApJ

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“…The current favored hypothesis for establishing this dichotomy is the formation of Jupiter, which acted as a physical barrier preventing mixing of grains between outer (CC-like) and inner (NC-like) regions of the disk (Kruijer et al 2017). The isotopic reservoir located in the outer solar system (CC-like material) carries excesses of neutron-rich Cr, Ti, Mo and Ni isotopes created in neutron-rich stellar environments (Nanne et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Xenon Isotopes Identify Large-scale Nucleosynthetic Heterogeneities across the Solar System

Avice

Moreira

Gilmour

2020

ApJ

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6 figures, 1 table total number of words: 5045 (all included) number of references: 47Abstract Nucleosynthetic isotopic anomalies in meteorites and planetary objects contribute to our understanding of the formation of the solar system. Isotope systematics of chondrites demonstrate the existence of a physical separation between isotopic reservoirs in the solar system.The isotopic composition of atmospheric xenon (Xe) indicates that its progenitor, U-Xe, is depleted in 134 Xe and 136 Xe isotopes relative to Solar or Chondritic end-members. This deficit supports the view that nucleosynthetic heterogeneities persisted during the Solar System formation. Measurements of xenon emitted from comet 67P/Churyumov-Gerasimenko (67P) identified a similar, but more extreme, deficit of cometary gas in these isotopes relative to Solar gas.Here we show that the data from 67P demonstrate that two distinct sources contributed xenon isotopes associated with the r-process to the solar system. The h-process contributed at least 29% (2s) of solar system 136 Xe.Mixtures of these r-process components and the s-process that match the heavy isotope signature of cometary Xe lead to depletions of the precursor of atmospheric Xe in p-only isotopes. Only the addition of pure p-process Xe to the isotopic mixture brings 124 Xe/ 132 Xe and 126 Xe/ 132 Xe ratios back to solar-like values. No pure p-process Xe has been detected in solar system material, and variation in p-process Xe isotopes is always correlated with variation in rprocess Xe isotopes. In the solar system, p-process incorporation from the interstellar medium happened before incorporation of r-process nuclides or material in the outer edge of the solar system carries a different mixture of presolar sources as have been preserved in parent bodies.

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GAUSS - genesis of asteroids and evolution of the solar system

et al. 2021

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The goal of Project GAUSS (Genesis of Asteroids and evolUtion of the Solar System) is to return samples from the dwarf planet Ceres. Ceres is the most accessible candidate of ocean worlds and the largest reservoir of water in the inner Solar System. It shows active volcanism and hydrothermal activities in recent history. Recent evidence for the existence of a subsurface ocean on Ceres and the complex geochemistry suggest past habitability and even the potential for ongoing habitability. GAUSS will return samples from Ceres with the aim of answering the following top-level scientific questions: What is the origin of Ceres and what does this imply for the origin of water and other volatiles in the inner Solar System? What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of dwarf planets? What are the astrobiological implications of Ceres? Is it still habitable today? What are the mineralogical connections between Ceres and our current collections of carbonaceous meteorites?

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Origin of the non-carbonaceous–carbonaceous meteorite dichotomy

Cited by 154 publications

References 48 publications

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Fingerprints of the Protosolar Cloud Collapse in the Solar System. II. Nucleosynthetic Anomalies in Meteorites

Xenon Isotopes Identify Large-scale Nucleosynthetic Heterogeneities across the Solar System

GAUSS - genesis of asteroids and evolution of the solar system

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