Hf–W mineral isochron for Ca,Al-rich inclusions: Age of the solar system and the timing of core formation in planetesimals

By C. Burkhardt, T. Kleine, B. Bourdon, H. Palme, J. Zipfel, J. Friedrich, Denton S. Ebel. 2008

148 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/d5b180d23a27527f714415137cbfe6ecc6062a1b

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In Astronomy and Astrophysics

1. A. Morbidelli
2. N. Dauphas
3. S. Raymond
4. T. Kleine
5. Kevin J. Walsh
6. C. Burkhardt
7. B. Bourdon
8. D. Nesvorný

In Geophysics

1. B. Bourdon
2. T. Kleine
3. A. Morbidelli
4. C. Burkhardt
5. N. Dauphas
6. H. Palme
7. A. Halliday
8. F. Nimmo

Citations in the corpus

• Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets (2009, background): “W isochrons involving high-Ca pyroxene and other silicates (e.g., olivine, melilite), such as for CAIs (Burkhardt et al., 2008) and angrites (Markowski et al., 2007; Kleine et al., 2008a), or co-genetic metal and silicate fractions, such as for H chondrites (Kleine et al., 2008b).”
• 26Al‐26Mg isotope systematics of the first solids in the early solar system (2013, unknown): “The Hf-W age difference between CAI (Burkhardt et al. 2008) and the quenched angrites (Kleine et al. 2012) is 4.2 0.6 Ma, which is in agreement with the Al-Mg age of the quenched angrites (Fig.”
• Building Terrestrial Planets (2012, background): “planetesimal formation starts at the same “time zero” in every region of the proto-planetary disk, where “time zero” is usually identified with the formation time of the first solids, the calcium-aluminium inclusions (CAIs, dated at 4.568 Gy ago; Bouvier et al. 2007; Burkhardt et al. 2008).”
• STATISTICAL STUDY OF THE EARLY SOLAR SYSTEM'S INSTABILITY WITH FOUR, FIVE, AND SIX GIANT PLANETS (2012, background): “A protoplanetary nebula typically disperses in ∼3-10 Myr after the birth of the star (Haisch et al. 2001), which for the Sun was probably contemporary to the formation of the first Solar System solids, 4.568 Gyr ago (Bouvier et al. 2007, Burkhardt et al. 2008).”
• A Perspective from Extinct Radionuclides on a Young Stellar Object: The Sun and Its Accretion Disk (2011, background): “The initial (182Hf/180Hf)0 ratio of 9.72 ± 0.44 × 10−5 is well established from measurements of refractory inclusions (Burkhardt et al. 2008), and the decay constant is 0.078 Myr−1 (Vockenhuber et al. 2004).”
• U-Pb chronology of the Solar System's oldest solids with variable 238 U/ 235 U (2010, methodology): “…et al. 2002, Bizzarro et al. 2004, Thrane et al. 2006, Amelin and Krot 2007, Bouvier et al. 2007, Connelly et al. 2008a, Jacobsen et al. 2008, Burkhardt et al. 2008, Bouvier and Wadhwa 2009, Krot et al. 2009, Nyquist et al. 2009, Villeneuve et al. 2009) using extinct 26 Al26 Mg and 182 Hf182…”
• Correlated accretion ages and ε54Cr of meteorite parent bodies and the evolution of the solar nebula (2014, unknown): “The initial e182W is 3.51 0.10 (Burkhardt et al. 2012) and the initial 182Hf/180Hf is (9.72 0.44) 9 10 5(Burkhardt et al. 2008).”
• Chronology of the angrite parent body and implications for core formation in protoplanets (2012, methodology): “The initial 182Hf/180Hf ratios of the analyzed angrites range from (7.15 ± 0.17) 10 5 to (4.02 ± 0.24) 10 5, corresponding to time intervals, DtCAI, between 3.9 and 11.3 Myr after CAI formation using the initial 182Hf/180Hf of CAIs of (9.72 ± 0.44) 10 5(Burkhardt et al., 2008).”
• 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”
• Astrophysics with Extraterrestrial Materials (2016, background): “Small variations are seen across different types of irons, but indications are that differentiation and core formation occurred over a period of ∼1 Myr after CAI formation (Kleine et al. 2002, Burkhardt et al. 2008, Kruijer et al. 2014).”