Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets

By T. Kleine, M. Touboul, B. Bourdon, F. Nimmo, K. Mezger, H. Palme, S. Jacobsen, Q. Yin, A. Halliday. 2009

545 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/716131869df6b10b78d49782d40ec6ec221a2e18

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Citations in the corpus

Abundance, distribution, and origin of 60Fe in the solar protoplanetary disk (2012, background): “ggesting a time of core formation of 4.6 Myr after CAI (Ghosh and McSween, 1998). For comparison, the 182Hf-182W system gives a very uncertain age of 3±6 Myr for core formation in the HED parentbody (Kleine et al., 2009). Fig. 7. ε60Ni (see Fig. 1 caption for notations) isotope evolution of the mant”
Astrophysics with Extraterrestrial Materials (2016, methodology): “The primary tool used to study the formation ages of these objects has been the 182Hf/182W system (Kleine et al. 2009), as this system is based on elements that partition differently into the metallic core and silicate mantle during differentiation.”
Turbulent Mixing of Metal and Silicate during Planet Accretion – and interpretation of the Hf-W chronometer (2010, unknown): “N50Myrs) (Kleine et al., 2009).”
A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk (2011, methodology): “One can also calculate the accretion timescale of Earth for an exponentially decaying rate of accretion (see Section 6), and the result is τ ~ 10 Myr (Jacobsen 2005, Kleine et al. 2009, Yin et al. 2002), which represents the time that Earth would have reached two-thirds of its present size.”
U-Pb chronology of the Solar System's oldest solids with variable 238 U/ 235 U (2010, methodology): “The cause of the apparent age difference between six Efremovka and Allende CAIs of ca. 4566.8 Ma, and two NWA 2364 and Vigarano CAIs of ca. 4568.4 Ma is unclear.”
Water delivery and giant impacts in the 'Grand Tack' scenario (2014, unknown): “The emerging data suggests substantially different timescales of accretion for different planets, with estimates of 30–100 Myr for Earth vs. 2–10 Myr for Mars (e.g. Halliday, 2000; Halliday and Kleine, 2006; Kleine et al., 2009; Nimmo and Kleine, 2007; Dauphas and Pourmand, 2011).”
Formation of planetary systems by pebble accretion and migration (2018, background): “The growth of the Earth likely took place over a timescale of several tens of millions of years based on the age constraints on the Moon-forming impact (Touboul et al. 2007; Kleine et al. 2009; Jacobson et al. 2014; Barboni et al. 2017).”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION (2011, background): “…the extent of chemical equilibration between the metals and silicates within the growing planet, measurements of the present-day ratios of Hf and W isotopes constrain the time scale for planet formation, including the timing of the proposed Moonforming impact (Jacobsen 2005; Kleine et al. 2009).”
Molybdenum isotope anomalies in meteorites: Constraints on solar nebula evolution and origin of the Earth (2011, background): “The largest anomalies were measured for some of the oldest objects, CAI A-ZH-5, while no anomalies were resolved for the terrestrial planets, which were fully accreted much later than the meteorite parent bodies (e.g., Kleine et al., 2009).”
Correlated accretion ages and ε54Cr of meteorite parent bodies and the evolution of the solar nebula (2014, methodology): “This approach has been applied to iron meteorites, ordinary chondrites, and CO chondrites, etc. (Scott 2007; Qin et al. 2008; Kleine et al. 2009; Kruijer et al. 2013).”
Building Terrestrial Planets (2012, background): “Moreover, they form too quickly compared with the timescale of tens of millions of years suggested for Earth by radioactive chronometers (Kleine et al. 2009).”
EVIDENCE FROM THE ASTEROID BELT FOR A VIOLENT PAST EVOLUTION OF JUPITER's ORBIT (2010, background): “Geochemical constraints (Touboul et al., 2007; Allegre et al., 2008; Kleine et al., 2009) and numerical modeling (Chambers and Wetherill, 1998; Chambers, 2001; Raymond et al., 2006; O’Brien et al., 2006; Hansen, 2009; Morishima et al., 2010) suggest that the terrestrial planets took 30–100 My to…”
A sawtooth-like timeline for the first billion years of lunar bombardment (2012, methodology): “Step I: First, we extrapolated the NI94 curve to 4.5 Gy, the approximate time of the Moon’s formation (Kleine et al., 2009).”
Chronology of the angrite parent body and implications for core formation in protoplanets (2012, methodology): “As evident from strong (182)W deficits in most magmatic iron meteorites, core formation in their parent bodies must have occurred within 1 Myr after formation of Ca,Al-rich inclusions (CAI) (Kleine et al., 2005a; Markowski et al., 2006; Scherstén et al., 2006; Burkhardt et al., 2008; Qin et al., 200”
Melting and differentiation of early-formed asteroids: The perspective from high precision oxygen isotope studies (2017, background): “Dating studies based on the decay of extinct 182Hf (t½ = 8.9 Myr) to 182W support such rapid accretion rates and indicate that the parent bodies of the magmatic iron meteorites formed as little as 100,000 years after calcium aluminium-rich inclusions (CAIs), which are the ear- liest dated Solar Syst”
HED Meteorites and Their Relationship to the Geology of Vesta and the Dawn Mission (2011, background): “However, Kleine et al. (2009) argued that the imprecisely defined isotopic ratios for average basaltic eucrites make the time of core formation more uncertain, and they calculated times of 3+6 Myr after CAIs.”