THE Hf-W ISOTOPIC SYSTEM AND THE ORIGIN OF THE EARTH AND MOON

By S. Jacobsen. 2005

211 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/bad419e99f47f2f7f12ea1a3eccca6a024296063

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Citations in the corpus

Ranges of Atmospheric Mass and Composition of Super-Earth Exoplanets (2008, background): “In our solar system, the accretion and metallic core segregation in the terrestrial planets occurred about 10 Myr after the formation of the solar system (Yin et al., 2002; Kleine et al., 2002; Jacobsen 2005).”
Water and astrobiology (2007, methodology): “…fashion over a period probably no longer than 30–50Myr following the onset of nebular condensation, based on Hf-W isotopic evidence that Earth’s core had formed by this time (Schoenberg et al., 2002; Yin et al., 2002; Kleine et al., 2002; Jacobsen, 2005, Halliday and Kleine, 2006; Halliday, 2006).”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, methodology): “The minimum time in which the Earth acquired 63% of its mass is 11 My (Yin et al., 2002; Jacobsen, 2005).”
Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets (2009, background): “However, for modeling purposes some authors (Harper and Jacobsen, 1996; Jacobsen, 2005; Nimmo and Agnor, 2006) also expressed 182W/184W relative to the W isotope composition of the CHondritic Uniform Res- ervoir (CHUR), as defined by the W isotope evolution of carbonaceous chondrites (Section 2.3).”
A Decreased Probability of Habitable Planet Formation around Low-Mass Stars (2007, unknown): “This increases to 20-50 Myr for Sun-like stars, consistent with estimates from Hf/W isotopic measurements (e.g., Jacobsen 2005).”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, methodology): “According to Hf-W isotope analysis, the earliest time the Moon-forming giant impact could have taken place, corresponds to the end of main-stage accretion at approximately 30 Myr (Kleine et al. 2002; Jacobsen 2005; Wood et al. 2006, Yu and Jacobsen 2011).”
FORMATION OF THE TERRESTRIAL PLANETS FROM A NARROW ANNULUS (2009, methodology): “Cosmochemical studies of radionuclides can provide valuable constraints on the timescale over which planets accumulate their mass, although the inferences are somewhat dependant on the details of the isotopes and methods used (e.g., Halliday 2004; Jacobsen 2005; Touboul et al. 2007).”
Hf-W thermochronometry: Closure temperature and constraints on the accretion and cooling history of the H chondrite parent body (2008, background): “planets (Harper and Jacobsen, 1996; Schoenberg et al., 2002; Yin et al., 2002; Halliday, 2004; Kleine et al., 2004b; Jacobsen, 2005; Nimmo and Agnor, 2006; Nimmo and Kleine, 2007) but its potential for dating chondrites and constraining the thermal evolution of their parent bodies has yet to be expl”
A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk (2011, methodology): “For Earth, one can directly use the output of N-body simulations to predict ε182W in the mantle (Jacobsen 2005, Nimmo & Agnor 2006, Nimmo et al. 2010), which can then be compared with the measured value of ~+2.”
The partitioning of trace elements between ilmenite, ulvospinel, armalcolite and silicate melts with implications for the early differentiation of the moon (2006, background): “The discussion on these matters has recently been revived by studies of Hf–W isotopes in lunar, terrestrial, and meteoritic rocks (Lee and Halliday, 1995; Lee et al., 1997, 2002; Kramers, 1998; Shearer and Newsom, 2000; Schoenberg et al., 2002; Yin et al., 2002; Shearer and Righter, 2003; Kleine et ”
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).”
Possible formation of ancient crust on Mars through magma ocean processes (2005, background): “formation of the terrestrial planets was complete has shortened from within 10 to 13 Myr [Blichert-Toft et al., 1999; Shih et al., 1999; Kleine et al., 2002], and for Mars, to less than 10 Myr after solar system formation [Yin et al., 2002; Jacobsen, 2005 ].”