Early core formation in asteroids and late accretion of chondrite parent bodies: Evidence from 182Hf-182W in CAIs, metal-rich chondrites, and iron meteorites

By T. Kleine, K. Mezger, H. Palme, E. Scherer, C. Münker. 2005

299 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/6f87e8423309f8d11d4f2efaf5860b5ff0cd53a4

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Citations in the corpus

Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets (2009, methodology): “…26Al was sufficiently abundant to melt early-formed (<1 Myr) planetesimals, whereas in the late-formed (>2 Myr) chondrite parent bodies too little 26Al remained to raise the temperatures high enough to cause large-scale melting and differentiation (Kleine et al., 2005b; Schérsten et al., 2006).”
The lunar magma ocean: Reconciling the solidification process with lunar petrology and geochronology (2011, background): “The initial results showing large 182W excess (Lee et al., 2002; Kleine et al., 2005; see ages b, c, and d in Fig.”
Molybdenum isotope anomalies in meteorites: Constraints on solar nebula evolution and origin of the Earth (2011, background): “…data for magmatic iron meteorites indicate that their parent bodies accreted within less than ~1 Ma after CAI formation (Burkhardt et al., 2008; Kleine et al., 2005; Qin et al., 2008; Scherstén et al., 2006), while the majority of chondrules formed 2–3 Ma after CAI formation, as indicated by…”
Chronology of the Solar System’s Oldest Solids (2008, background): “…may, in turn, reflect their early incorporation into the parent bodies of differentiated meteorites, given that the accretion of differentiated planetesimals is commonly believed to have predated that of chondrite parent bodies (Bizzarro et al. 2005; Baker et al. 2005; Kleine et al. 2005).”
Emergence of a Habitable Planet (2007, background): “The latest data for iron meteorites provide evidence that accretion and core formation were very short-lived (Kleine et al. 2005a; Markowski et al. 2006; Scherstén et al. 2006).”
Broad bounds on Earth’s accretion and core formation constrained by geochemical models (2010, background): “This assumption seems reasonable, given the evidence for very early differentiation of meteorite parent bodie”
Hf–W mineral isochron for Ca,Al-rich inclusions: Age of the solar system and the timing of core formation in planetesimals (2008, methodology): “Application of 182Hf–182W chronometry to iron meteorites, however, has challenged this classical model for the accretion and differentiation of asteroids (Kleine et al., 2005; Markowski et al., 2006b; Schérsten et al., 2006; Qin et al., 2008b).”
Nickel isotope heterogeneity in the early Solar System (2008, background): “Samples that have ε182W more negative than the initial ε182W of the Solar System, −3.5±0.2 (Kleine et al., 2005) are clearly influenced by spallation and these values are italicised. g NIST SRM986 col refers to a solution of the NBS986 Ni isotope standard that was processed through the chemical…”
Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation (2010, background): “Hf/W chronometry indicates that these cores formed within 0–3 million years (Ma) after the formation of calcium aluminum inclusions (CAIs) (Kleine et al. 2005).”
Chondrule formation during planetesimal accretion (2011, background): “This agrees with radioisotopic (Bizzarro et al., 2005; Kleine et al., 2005; Lee and Halliday, 1996) and petrological (Keil, 2000) records.”
Chronology of the angrite parent body and implications for core formation in protoplanets (2012, background): “…of igneous achondrites are more difficult to interpret, as they reflect not only Hf/W fractionation during core formation but also additional fractionations during later melting and metamorphic processes (Quitté et al., 2000; Kleine et al., 2005b; Markowski et al. 2007; Kleine et al., 2009).”
A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk (2011, background): “ERT FIGURE 6 HERE> Figure 6 Constraints from short-lived radionuclides on the timing of primary accretion. Relative ages are derived from 182Hf for magmatic iron meteorites (Burkhardt et al. 2008; Kleine et al. 2005, 2009; Markowski et al. 2006, 2007; Qin et al. 2008), 26Al for chondrules [total ”
Correlated accretion ages and ε54Cr of meteorite parent bodies and the evolution of the solar nebula (2014, background): “The early accretion of differentiated meteorite parent bodies compared with the accretion of chondrite parent bodies is now well established (Bizzarro et al. 2005; Kleine et al. 2005; Hevey and Sanders 2006).”