Hf–W evidence for rapid differentiation of iron meteorite parent bodies

Scherstén, Anders; Elliott, Tim; Hawkesworth, C. J.; Russell, S. S.; Masarik, J.

doi:10.1016/j.epsl.2005.11.025

Cited by 178 publications

(145 citation statements)

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“…As is evident from strong 182 W deficits in magmatic iron meteorites, core formation in their parent bodies was a very early process (Kleine et al 2005;Markowski et al 2006aMarkowski et al , 2006bScherstén et al 2006;Qin et al 2008a). Surprisingly, however, most iron meteorites exhibit 182 W/ 184 W lower than the solar system initial.…”

Section: Introductionmentioning

confidence: 99%

Nucleosynthetic Tungsten Isotope Anomalies in Acid Leachates of the Murchison Chondrite: Implications for Hafnium-Tungsten Chronometry

Burkhardt

Kleine

Dauphas

et al. 2012

ApJ

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Section: Introductionmentioning

confidence: 99%

Nucleosynthetic Tungsten Isotope Anomalies in Acid Leachates of the Murchison Chondrite: Implications for Hafnium-Tungsten Chronometry

Burkhardt

Kleine

Dauphas

et al. 2012

ApJ

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“…The parent body of angrites is 4564.42 ± 0.12 Ma old (Amelin 2008) and Quitté et al (2010) determined that its initial 60 Fe/ 56 Fe ratio is ≈(3.1 ± 0.8) × 10 −9 . Although tungsten isotope evidence (Schersten et al 2006;Qin et al 2008) indicates that most iron meteorites are formed within a few Ma of CAIs, they show no evidence of having 60 Ni excesses (Markowski et al 2006). The exact ages of these samples, however, remain poorly determined.…”

Section: Introductionmentioning

confidence: 97%

THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA

Moynier

Blichert‐Toft

Wang

et al. 2011

ApJ

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No 60 Ni or 61 Ni anomalies have been detected in troilite inclusions from Muonionalusta, a 4565.3 ± 0.1 Ma old IVA iron meteorite, to the level of the analytical precision of 10 ppm. Because Muonionalusta troilite is very old, has a high Fe/Ni ratio, and is free of 61 Ni anomalies, it is the ideal material in which to search for potential excesses of 60 Ni produced by the decay of 60 Fe (t 1/2 = 2.62 Ma). The 60 Ni/ 58 Ni and Fe/Ni ratios (up to 1680) measured here imply an upper limit for the initial 60 Fe/ 56 Fe for the Muonionalusta troilite of 3 × 10 −9 . Assuming that 60 Fe was homogeneously distributed across the nebula, this result suggests that the solar system initial 60 Fe/ 56 Fe ratio was less than 5 × 10 −9 , which is lower than previously measured by at least a factor of 50.

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“…Samples were analyzed only once, and the ratios are reported as relative deviations from the mass-bias corrected NIST 3163 tungsten reference material in the μ-notation (10 6 deviations). A blank correction (17,18,35,36).…”

Section: Methodsmentioning

confidence: 99%

¹⁸² Hf– ¹⁸² W age dating of a ²⁶ Al-poor inclusion and implications for the origin of short-lived radioisotopes in the early Solar System

Holst

Olsen

Paton

et al. 2013

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

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Refractory inclusions [calcium–aluminum-rich inclusions, (CAIs)] represent the oldest Solar System solids and provide information regarding the formation of the Sun and its protoplanetary disk. CAIs contain evidence of now extinct short-lived radioisotopes (e.g., 26 Al, 41 Ca, and 182 Hf) synthesized in one or multiple stars and added to the protosolar molecular cloud before or during its collapse. Understanding how and when short-lived radioisotopes were added to the Solar System is necessary to assess their validity as chronometers and constrain the birthplace of the Sun. Whereas most CAIs formed with the canonical abundance of 26 Al corresponding to 26 Al/ 27 Al of ∼5 × 10 −5 , rare CAIs with fractionation and unidentified nuclear isotope effects (FUN CAIs) record nucleosynthetic isotopic heterogeneity and 26 Al/ 27 Al of <5 × 10 −6 , possibly reflecting their formation before canonical CAIs. Thus, FUN CAIs may provide a unique window into the earliest Solar System, including the origin of short-lived radioisotopes. However, their chronology is unknown. Using the 182 Hf– 182 W chronometer, we show that a FUN CAI recording a condensation origin from a solar gas formed coevally with canonical CAIs, but with 26 Al/ 27 Al of ∼3 × 10 −6 . The decoupling between 182 Hf and 26 Al requires distinct stellar origins: steady-state galactic stellar nucleosynthesis for 182 Hf and late-stage contamination of the protosolar molecular cloud by a massive star(s) for 26 Al. Admixing of stellar-derived 26 Al to the protoplanetary disk occurred during the epoch of CAI formation and, therefore, the 26 Al– 26 Mg systematics of CAIs cannot be used to define their formation interval. In contrast, our results support 182 Hf homogeneity and chronological significance of the 182 Hf– 182 W clock.

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Hf–W evidence for rapid differentiation of iron meteorite parent bodies

Cited by 178 publications

References 57 publications

Nucleosynthetic Tungsten Isotope Anomalies in Acid Leachates of the Murchison Chondrite: Implications for Hafnium-Tungsten Chronometry

Nucleosynthetic Tungsten Isotope Anomalies in Acid Leachates of the Murchison Chondrite: Implications for Hafnium-Tungsten Chronometry

THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA

¹⁸² Hf– ¹⁸² W age dating of a ²⁶ Al-poor inclusion and implications for the origin of short-lived radioisotopes in the early Solar System

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Hf–W evidence for rapid differentiation of iron meteorite parent bodies

Cited by 178 publications

References 57 publications

Nucleosynthetic Tungsten Isotope Anomalies in Acid Leachates of the Murchison Chondrite: Implications for Hafnium-Tungsten Chronometry

Nucleosynthetic Tungsten Isotope Anomalies in Acid Leachates of the Murchison Chondrite: Implications for Hafnium-Tungsten Chronometry

THE ELUSIVE60Fe IN THE SOLAR NEBULA

182 Hf– 182 W age dating of a 26 Al-poor inclusion and implications for the origin of short-lived radioisotopes in the early Solar System

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THE ELUSIVE⁶⁰Fe IN THE SOLAR NEBULA

¹⁸² Hf– ¹⁸² W age dating of a ²⁶ Al-poor inclusion and implications for the origin of short-lived radioisotopes in the early Solar System