Correlated accretion ages and ε<sup>54</sup>Cr of meteorite parent bodies and the evolution of the solar nebula

Sugiura, N.; Fujiya, Wataru

doi:10.1111/maps.12292

Cited by 136 publications

(141 citation statements)

References 67 publications

(174 reference statements)

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“…[75] Estimates of the accretion times of the chondrite parent bodies (modified after [72]). All the chondrites have avoided melting, but they experienced sufficient lithification as a result of metamorphism and/or aqueous alteration to be robust enough to survive impacts and atmospheric entry.…”

Section: Meteorites In Briefmentioning

confidence: 99%

The origin of inner Solar System water

Alexander¹

2017

Phil. Trans. R. Soc. A.

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Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H 2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3–7 AU in the Grand Tack model) and possibly close to where they are found today. This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.

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Section: Meteorites In Briefmentioning

confidence: 99%

The origin of inner Solar System water

Alexander¹

2017

Phil. Trans. R. Soc. A.

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“…This could reflect temporal or spatial variations in the distribution of components with a primordial molecular cloud signature in the protoplanetary disk. However, CR, CI, and CM chondrites record comparable aqueous alteration ages (39). This observation suggests that the accretion region of CR chondrites was spatially isolated from that of CI and CM chondrites.…”

Section: Accretion Region Of Metal-rich Carbonaceous Chondritesmentioning

confidence: 75%

Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

Kooten

Wielandt

Schiller

et al. 2016

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

173

124

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The short-lived 26 Al radionuclide is thought to have been admixed into the initially 26 Al-poor protosolar molecular cloud before or contemporaneously with its collapse. Bulk inner Solar System reservoirs record positively correlated variability in mass-independent 54 Cr and 26 Mg*, the decay product of 26 Al. This correlation is interpreted as reflecting progressive thermal processing of infalling 26 Al-rich molecular cloud material in the inner Solar System. The thermally unprocessed molecular cloud matter reflecting the nucleosynthetic makeup of the molecular cloud before the last addition of stellar-derived 26 Al has not been identified yet but may be preserved in planetesimals that accreted in the outer Solar System. We show that metal-rich carbonaceous chondrites and their components have a unique isotopic signature extending from an inner Solar System composition toward a 26 Mg*-depleted and 54 Cr-enriched component. This composition is consistent with that expected for thermally unprocessed primordial molecular cloud material before its pollution by stellar-derived 26 Al. The 26 Mg* and 54 Cr compositions of bulk metal-rich chondrites require significant amounts (25-50%) of primordial molecular cloud matter in their precursor material. Given that such high fractions of primordial molecular cloud material are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted beyond the orbits of the gas giants. The lack of evidence for this material in other chondrite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from the early formation of gas giants. molecular cloud | outer Solar System | metal-rich chondrites | isotopes | chondrite accretion regions L ow-mass stars like our Sun form by the gravitational collapse of the densest parts of molecular clouds comprising stellarderived dust and gas. Collapsing clouds swiftly evolve into deeply embedded protostars that rapidly accrete material from their surrounding envelopes via a protoplanetary disk (1), in which planetesimals and planetary embryos form over timescales of several million years (2). Chondritic meteorites (chondrites) are fragments of early-formed planetesimals that avoided melting and differentiation and, therefore, provide a record of the earliest evolutionary stages of the Sun and its protoplanetary disk. Most chondrites contain calcium−aluminum-rich inclusions (CAIs) and chondrules, which formed by high-temperature processes that included evaporation, condensation, and melting during short-lived heating events (3). CAIs represent the oldest dated solids and, thus, define the age of the Solar System at 4,567.3 ± 0.16 Ma (4). It is inferred that CAIs formed near the proto-Sun during a brief time interval (<0

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“…) and the upper age limits of the accretion ages of these bodies or their precursors. Accretion ages for the ureilite and howardite–eucrite–diogenite (HED) parent bodies are either derived from thermal models assuming initial 26 Al/ 27 Al abundances similar to that of calcium‐aluminum‐rich inclusions (CAIs) in CV‐type chondrites (Sugiura and Fujiya ; Goodrich et al. ) or estimates of the initial 26 Al/ 27 Al abundance of solids in the inner disk that have nucleosynthetic signatures akin to meteorites originating from the ureilite and HED parent bodies (Larsen et al.…”

Section: Discussionmentioning

confidence: 99%

“… Upper accretion ages for ureilite and HED parent bodies calculated using an CAI‐like initial 26 Al (Sugiura and Fujiya ; Goodrich et al. ). …”

Section: Discussionmentioning

confidence: 99%

Testing accretion mechanisms of the H chondrite parent body utilizing nucleosynthetic anomalies

Pedersen

Schiller

Connelly

et al. 2019

Meteorit & Planetary Scien

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Planetary bodies a few hundred kilometers in radii are the precursors to larger planets but it is unclear whether these bodies themselves formed very rapidly or accreted slowly over several millions of years. Ordinary H chondrite meteorites provide an opportunity to investigate the accretion time scale of a small planetary body given that variable degrees of thermal metamorphism present in H chondrites provide a proxy for their stratigraphic depth and, therefore, relative accretion times. We exploit this feature to search for nucleosynthetic isotope variability of 54Cr, which is a sensitive tracer of spatial and temporal variations in the protoplanetary disk's solids, between 17 H chondrites covering all petrologic types to obtain clues about the parent body accretionary rate. We find no systematic variability in the mass‐biased corrected abundances of 53Cr or 54Cr outside of the analytical uncertainties, suggesting very rapid accretion of the H chondrite parent body consistent with turbulent accretion. By utilizing the μ54Cr–planetary mass relationship observed between inner solar system planetary bodies, we calculate that the H chondrite accretion occurred at 1.1 ± 0.4 or 1.8 ± 0.2 Myr after the formation of calcium‐aluminum‐rich inclusions (CAIs), assuming either the initial 26Al/27Al abundance of inner solar system solids determined from angrite meteorites or CAIs from CV chondrites, respectively. Notably, these ages are in agreement with age estimates based on the parent bodies’ thermal evolution when correcting these calculations to the same initial 26Al/27Al abundance, reinforcing the idea of a secular evolution in the isotopic composition of inner disk solids.

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Correlated accretion ages and ε⁵⁴Cr of meteorite parent bodies and the evolution of the solar nebula

Cited by 136 publications

References 67 publications

The origin of inner Solar System water

The origin of inner Solar System water

Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

Testing accretion mechanisms of the H chondrite parent body utilizing nucleosynthetic anomalies

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Correlated accretion ages and ε54Cr of meteorite parent bodies and the evolution of the solar nebula

Cited by 136 publications

References 67 publications

The origin of inner Solar System water

The origin of inner Solar System water

Isotopic evidence for primordial molecular cloud material in metal-rich carbonaceous chondrites

Testing accretion mechanisms of the H chondrite parent body utilizing nucleosynthetic anomalies

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Product

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Correlated accretion ages and ε⁵⁴Cr of meteorite parent bodies and the evolution of the solar nebula