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

By A. Schersten, T. Elliott, C. Hawkesworth, S. Russell, J. Masarik. 2006

183 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/1e5af0bd1a7cbc4dc511eea261930153fa1bbb10

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In Astronomy and Astrophysics

1. L. Elkins‐Tanton
2. T. Kleine
3. B. Bourdon
4. E. Scott
5. C. Burkhardt
6. A. Halliday
7. F. Nimmo
8. H. Palme

In Geophysics

1. B. Bourdon
2. T. Kleine
3. E. Scott
4. H. Palme
5. L. Elkins‐Tanton
6. C. Burkhardt
7. F. Nimmo
8. Q. Yin

Citations in the corpus

• Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets (2009, background): “…182W/184W reported for iron meteorites does not provide a robust estimate for the initial 182W/184W of the solar system but rather reflects the effects of interaction with thermal neutrons (Masarik, 1997; Leya et al., 2003; Kleine et al., 2005b; Markowski et al., 2006b; Schérsten et al., 2006).”
• Molybdenum isotope anomalies in meteorites: Constraints on solar nebula evolution and origin of the Earth (2011, background): “Hafnium–tungsten 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 ind”
• Modeling fractional crystallization of group IVB iron meteorites (2008, background): “Tungsten isotope studies have shown that the parental metallic liquids to these meteorites segregated from silicates within several million years of the formation of the solar system (Horan et al., 1998; Scherstén et al., 2006).”
• Chondrules and the Protoplanetary Disk (2011, background): “However, the low 182W/184W ratios of irons indicating metalsilicate fractionation in <1–1.5 Myr are entirely consistent with the 0.7 Myr half-life of 26Al, and they exclude a major role for impact heating (Scherstén et al. 2006).”
• Nickel isotope heterogeneity in the early Solar System (2008, methodology): “This is unexpected, given the rapid timescales of planetesimal iron meteorite formation implied byW isotope studies (Kleine et al., 2005; Scherstén et al., 2006; Markowski et al., 2006a).”
• Hf–W mineral isochron for Ca,Al-rich inclusions: Age of the solar system and the timing of core formation in planetesimals (2008, background): “Most iron meteorites have relatively long exposure times, such that in most cases their e182W values were significantly lowered to values more negative than the initial e182W of CAIs (Kleine et al., 2005; Markowski et al., 2006b; Schérsten et al., 2006).”
• 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).”
• Magma oceans in the inner solar system (2012, background): “Their isotopic composition indicates that a majority of them solidified less than 1 Ma after the first solids in the solar system formed Scherstén et al. (2006), indicating that scores of bodies accreted fast, melted internally, and differentiated.”
• Chronology of the angrite parent body and implications for core formation in protoplanets (2012, methodology): “The matrix containing mostly Ti, Zr and Hf was eluted using 10 ml 1 M HCl–2% H2O2 (following Quitté et al., 2000; Scherstén et al., 2006).”