Early planetesimal melting from an age of 4.5662 Gyr for differentiated meteorites

Baker, Joel A.; Bizzarro, Martin; Wittig, N.; Connelly, James N.; Haack, H.

doi:10.1038/nature03882

Cited by 255 publications

(226 citation statements)

References 21 publications

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“…Angrites are among the oldest basaltic rocks in the Solar System (Baker et al, 2005;Nyquist et al, 2009;Dauphas and Chaussidon, 2011). Only 19 angrites are recognized.…”

Section: Sample Descriptionsmentioning

confidence: 99%

Iron isotope fractionation in planetary crusts

Wang

Moynier

Dauphas

et al. 2012

Geochimica et Cosmochimica Acta

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We present new high precision iron isotope data (d 56 Fe vs. IRMM-014 in per mil) for four groups of achondrites: one lunar meteorite, 11 martian meteorites, 32 howardite-eucrite-diogenite meteorites (HEDs), and eight angrites. Angrite meteorites are the only planetary materials, other than Earth/Moon system, significantly enriched in the heavy isotopes of Fe compared to chondrites (by an average of +0.12& in d 56 Fe). While the reason for such fractionation is not completely understood, it might be related to isotopic fractionation by volatilization during accretion or more likely magmatic differentiation in the angrite parent-body. We also report precise data on martian and HED meteorites, yielding an average d 56 Fe of 0.00 ± 0.01&. Stannern-trend eucrites are isotopically heavier by +0.05& in d 56 Fe than other eucrites. We show that this difference can be ascribed to the enrichment of heavy iron isotopes in ilmenite during igneous differentiation. Preferential dissolution of isotopically heavy ilmenite during remelting of eucritic crust could have generated the heavy iron isotope composition of Stannern-trend eucrites. This supports the view that Stannern-trend eucrites are derived from main-group eucrite source magma by assimilation of previously formed asteroidal crust.These new results show that iron isotopes are not only fractionated in terrestrial and lunar basalts, but also in two other differentiated planetary crusts. We suggest that igneous processes might be responsible for the iron isotope variations documented in planetary crusts.

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“…Angrites are among the oldest basaltic rocks in the Solar System (Baker et al, 2005;Nyquist et al, 2009;Dauphas and Chaussidon, 2011). Only 19 angrites are recognized.…”

Section: Sample Descriptionsmentioning

confidence: 99%

Iron isotope fractionation in planetary crusts

Wang

Moynier

Dauphas

et al. 2012

Geochimica et Cosmochimica Acta

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“…Accordingly, several groups have developed a wide range of thermal models of planetesimals with short-lived radioactive nuclides (mainly 26 Al but also 60 Fe) as the main heat source (e.g., Miyamoto et al 1981;Miyamoto 1991;Grimm and McSween 1993;Bennett and McSween 1996;Akridge et al 1998;Merk et al 2002;Ghosh et al 2003;Tachibana & Huss 2003;Trieloff et al 2003;Bizzarro et al 2005;Baker et al 2005;Mostefaoui et al 2005;Hevey & Sanders 2006;Sahijpal et al 2007;Harrison & Grimm 2010;Elkins-Tanton et al 2011;Henke et al 2012aHenke et al , 2012bNeumann et al 2012;Monnereau et al 2013). In the context of ordinary chondrite parent bodies, such models predict an onion-shell structure (Trieloff et al 2003;Ghosh et al 2006;Henke et al 2012aHenke et al , 2012bHenke et al , 2013Wood 2003, and references therein), where all petrologic types formed on the same parent body with type 3 OCs being representative of the crust and type 6 OCs being representative of the core.…”

Section: Introductionmentioning

confidence: 99%

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Vernazza

Zanda

Binzel

et al. 2014

ApJ

125

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Although petrologic, chemical, and isotopic studies of ordinary chondrites and meteorites in general have largely helped establish a chronology of the earliest events of planetesimal formation and their evolution, there are several questions that cannot be resolved via laboratory measurements and/or experiments alone. Here, we propose the rationale for several new constraints on the formation and evolution of ordinary chondrite parent bodies (and, by extension, most planetesimals) from newly available spectral measurements and mineralogical analysis of main-belt S-type asteroids (83 objects) and unequilibrated ordinary chondrite meteorites (53 samples). Based on the latter, we suggest that spectral data may be used to distinguish whether an ordinary chondrite was formed near the surface or in the interior of its parent body. If these constraints are correct, the suggested implications include that: (1) large groups of compositionally similar asteroids are a natural outcome of planetesimal formation and, consequently, meteorites within a given class can originate from multiple parent bodies; (2) the surfaces of large (up to ∼200 km) S-type main-belt asteroids mostly expose the interiors of the primordial bodies, a likely consequence of impacts by small asteroids (D < 10 km) in the early solar system; (3) the duration of accretion of the H chondrite parent bodies was likely short (instantaneous or in less than ∼10 5 yr, but certainly not as long as 1 Myr); (4) LL-like bodies formed closer to the Sun than H-like bodies, a possible consequence of the radial mixing and size sorting of chondrules in the protoplanetary disk prior to accretion.

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“…[7,9,11,14,15,17,19] Nevertheless, debate continues regarding: (1) whether the earth has a chondritic Mg isotopic composition or not, [7][8][9]13,18,20] and (2) the accuracy of Mg isotopic compositions reported by different labs for certain geostandards, such as BCR-1, BCR-2 and San Carlos olivine. [5,9,10,12,13,16,18,[20][21][22][23][24][25] Both debates may reflect the presence of MC-ICP-MS analytical artifacts in high-precision Mg isotopic analyses conducted at different laboratories. [7][8][9]18,20] Analyses of geostandards BCR-1 and BCR-2 in different laboratories yielded significantly different Mg isotopic compositions ( Fig.…”

mentioning

confidence: 99%

Homogeneous magnesium isotopic composition of seawater: an excellent geostandard for Mg isotope analysis

Ling

Sedaghatpour

Teng

et al. 2011

Rapid Comm Mass Spectrometry

145

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The magnesium (Mg) isotopic compositions of 40 seawater samples from the Gulf of Mexico and of one seawater sample from the southwest Hawaii area were determined by multi-collector inductively coupled plasma mass spectrometry (MC-ICP-MS) to investigate the homogeneity of Mg isotopes in seawater. The results indicate that the Mg isotopic composition of seawater from the Gulf of Mexico is homogeneous, both vertically and horizontally, with average values for d 25 Mg = À0.43 AE 0.06 (2SD, n = 90). The magnesium isotopic composition of seawater is principally controlled by river water input, carbonate precipitation and oceanic hydrothermal interactions. The homogeneous Mg isotopic composition of seawater indicates a steady-state budget in terms of Mg isotopes in oceans, consistent with a long Mg residence time (~13 Ma). Considering that seawater is homogeneous, readily available in large amounts, can be easily accessed and processed for isotopic analysis, and has an isotopic composition near the middle of the natural range of variation, it is an excellent geostandard for accuracy assessment to rule out analytical artifacts during high-precision Mg isotopic analysis.

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Early planetesimal melting from an age of 4.5662 Gyr for differentiated meteorites

Cited by 255 publications

References 21 publications

Iron isotope fractionation in planetary crusts

Iron isotope fractionation in planetary crusts

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

Homogeneous magnesium isotopic composition of seawater: an excellent geostandard for Mg isotope analysis

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