182Hf-182W isotope systematics of chondrites, eucrites, and martian meteorites: Chronology of core formation and early mantle differentiation in Vesta and Mars

By T. Kleine, K. Mezger, C. Münker, H. Palme, A. Bischoff. 2004

311 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/6053ac95593a042f9ff07e32f633e09ed58f63bd

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Citations in the corpus

Emergence of a Habitable Planet (2007, background): “The most recent data for martian meteorites (Kleine et al. 2004; Foley et al. 2005) confirms earlier evidence (Lee and Halliday 1997) that accretion and core formation on Mars were fast.”
HED Meteorites and Their Relationship to the Geology of Vesta and the Dawn Mission (2011, background): “13b; Kleine et al. 2004 and Wadhwa et al. 2006) suggests that rapid core formation occurred 0.9+0.3 Myr before silicate (crust-mantle) differentiation, at 4563.2 +1.4 Ma.”
Magma oceans in the inner solar system (2012, background): “Mars likely formed before Earth and the Moon were in their current states (Kleine et al. 2004).”
Evidence for Mo isotope fractionation in the solar nebula and during planetary differentiation (2014, methodology): “Subsequently, any remaining Fe, Ni and a large part of the Ru was separated from Mo on an anion exchange resin (Bio-Rad AG1-X8) with 1 M HF, while Ti, Zr, Hf and W were eluted using different HCl–HF mixtures (Kleine et al., 2004).”
Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets (2009, methodology): “The two-stage W model ages for the formation of the martian core reported in the recent literature range from 3 to 12 Myr after CAI formation (Kleine et al., 2004a; Foley et al., 2005; Nimmo and Kleine, 2007).”
Hf–W mineral isochron for Ca,Al-rich inclusions: Age of the solar system and the timing of core formation in planetesimals (2008, methodology): “The accuracy of the measurements was monitored by analyzing some carbonaceous chondrites, all of which were consistent with the previously determined value of 1.9 ± 0.1 e182W (Kleine et al., 2004).”
Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation (2010, background): “Spectroscopic observations indicate that Vesta has a basaltic surface (McCord et al. 1970) and Hf/W chronometry of HED meteorites indicates it formed a metallic core within 3–4 Ma of solar system formation (Kleine et al. 2004).”
Chronology of the angrite parent body and implications for core formation in protoplanets (2012, methodology): “The separation of W from the unspiked aliquots initially followed our previously established techniques [labeled method A in Table 2 (Kleine et al., 2002, 2004; Burkhardt et al., 2008; Touboul et al., 2009)] but during the later course of this study a newly developed technique was used (labeled…”