Stable isotopes and the noncarbonaceous derivation of ureilites, in common with nearly all differentiated planetary materials

Warren, P. H.

doi:10.1016/j.gca.2011.09.011

Cited by 93 publications

(96 citation statements)

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“…A third component, possibly the complementary (partial) metallic liquid, might also be involved, the origin of which remains unsolved. A carbonaceous chondrite derivation of ureilites, however, has recently been brought into question by reviewing ureilite stable isotope systematics and mineralogical aspects (Warren ). Goodrich et al.…”

Section: Discussionmentioning

confidence: 99%

Si‐bearing metal and niningerite in Almahata Sitta fine‐grained ureilites and insights into the diversity of metal on the ureilite parent body

Horstmann

Humayun

Fischer-Gödde

et al. 2014

Meteorit & Planetary Scien

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A detailed mineralogical and chemical study of Almahata Sitta fine-grained ureilites was performed to shed light on the origin of these lithologies and their sulfide and metal. The Almahata Sitta fine-grained ureilites (silicates <30 lm grain size) show textural and chemical evidence for severe impact smelting as described for other fine-grained ureilites. Highly reduced areas in Almahata Sitta finegrained ureilites show large (up to $ 1 mm) Si-bearing metal grains (up to $ 4.5 wt% Si) and niningerite [Mg >0.5, (Mn,Fe) <0.5 S] with some similarities to the mineralogy of enstatite (E) chondrites. Overall, metal grains show a large compositional variability in Ni and Si concentrations. Niningerite grains probably formed as a by-product of smelting via sulfidation. The large Si-Ni variation in fine-grained ureilite metal could be the result of variable degrees of reduction during impact smelting, inherited from coarsegrained ureilite precursors, or a combination of both. Large Si-bearing metal grains probably formed via coalescence of existing and newly formed metal during impact smelting. Bulk and in situ siderophile trace element abundances indicate three distinct populations of (1) metal crystallized from partial melts in MS-20, (2) metal resembling bulk chondritic compositions in MS-165, and (3) residual metal in MS-168. Almahata Sitta fine-grained ureilites developed their distinctive mineralogy due to severe reduction during smelting. Despite the presence of E chondrite and ureilite stones in the Almahata Sitta fall, a mixing relation of E chondrites or their constituents and ureilite material in Almahata Sitta can be ruled out based on isotopic, textural, and mineral-chemical reasons.

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Section: Discussionmentioning

confidence: 99%

Si‐bearing metal and niningerite in Almahata Sitta fine‐grained ureilites and insights into the diversity of metal on the ureilite parent body

Horstmann

Humayun

Fischer-Gödde

et al. 2014

Meteorit & Planetary Scien

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“…; Qin et al. ; Warren ). This seems to be mainly due to contributions of CAIs and water ice, which affect strongly the bulk Δ 17 O, but not the ε 54 Cr.…”

Section: Cr Anomalies In Caismentioning

confidence: 99%

“…). The 54 Cr anomalies in bulk meteorites may have resulted from spatial (e.g., Warren ) or temporal large‐scale (of the order of 1 AU or larger) heterogeneity of the solar nebula. But destruction of a fraction of isotopically anomalous grains in parent bodies by aqueous alteration (Yokoyama et al.…”

Section: Introductionmentioning

confidence: 99%

Correlated accretion ages and ε⁵⁴Cr of meteorite parent bodies and the evolution of the solar nebula

Sugiura

Fujiya

2014

Meteorit & Planetary Scien

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Abstract-We look at the relationship between the value of e 54 Cr in bulk meteorites and the time (after calcium-aluminum-rich inclusion, CAI) when their parent bodies accreted. To obtain accretion ages of chondrite parent bodies, we estimated the maximum temperature reached in the insulated interior of each parent body, and estimated the initial 26 Al/ 27 Al for this temperature to be achieved. This initial 26 Al/ 27 Al corresponds to the time (after CAI formation) when cold accretion of the parent body would have occurred, assuming 26 Al/ 27 Al throughout the solar system began with the canonical value of 5.2 9 10 À5 . In cases of iron meteorite parent bodies, achondrite parent bodies, and carbonaceous chondrite parent bodies, we use published isotopic ages of events (such as core formation, magma crystallization, and growth of secondary minerals) in each body's history to obtain the probable time of accretion. We find that e 54 Cr correlates with accretion age: the oldest accretion ages (1 AE 0.5 Ma) are for iron and certain other differentiated meteorites with e 54 Cr of À0.75 AE 0.5, and the youngest ages (3.5 AE 0.5 Ma) are for hydrated carbonaceous chondrites with e 54 Cr values of 1.5 AE 0.5. Despite some outliers (notably Northwest Africa [NWA] 011 and Tafassasset), we feel that the correlation is significant and we suggest that it resulted from late, localized injection of dust with extremely high e 54 Cr.

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“…A protolith with S and Fe abundances similar to average CM can account for the ureilite features, but this solution is not unique. Notice that the protolith of the ureilites is not a known carbonaceous chondrite (Warren, 2011). tional melting), all melting happens at the eutectic until either metal or troilite is exhausted. The effect on the isotopic compositions of the residues can be easily estimated.…”

Section: Origin Of the High δ 56 Fe Values In Ureilitesmentioning

confidence: 99%

Early stages of core segregation recorded by Fe isotopes in an asteroidal mantle

Barrat

Rouxel

Wang

et al. 2015

Earth and Planetary Science Letters

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Available online xxxx Editor: B. Marty Keywords: iron isotopes achondrite ureilite coreUreilite meteorites are achondrites that are debris of the mantle of a now disrupted differentiated asteroid rich in carbon. They provide a unique opportunity to study the differentiation processes of such a body. We analyzed the iron isotopic compositions of 30 samples from the Ureilite Parent Body (UPB) including 29 unbrecciated ureilites and one ureilitic trachyandesite (ALM-A) which is at present the sole large crustal sample of the UPB. The δ 56 Fe of the whole rocks fall within a restricted range, from 0.01 to 0.11h, with an average of +0.056 ± 0.008h, which is significantly higher than that of chondrites.We show that this difference can be ascribed to the segregation of S-rich metallic melts at low degrees of melting at a temperature close to the Fe-FeS eutectic, and certainly before the onset of the melting of the silicates (<1100 • C), in agreement with the marked S depletions, and the siderophile element abundances of the ureilites. These results point to an efficient segregation of S-rich metallic melts during the differentiation of small terrestrial bodies.

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Stable isotopes and the noncarbonaceous derivation of ureilites, in common with nearly all differentiated planetary materials

Cited by 93 publications

References 93 publications

Si‐bearing metal and niningerite in Almahata Sitta fine‐grained ureilites and insights into the diversity of metal on the ureilite parent body

Si‐bearing metal and niningerite in Almahata Sitta fine‐grained ureilites and insights into the diversity of metal on the ureilite parent body

Correlated accretion ages and ε⁵⁴Cr of meteorite parent bodies and the evolution of the solar nebula

Early stages of core segregation recorded by Fe isotopes in an asteroidal mantle

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Stable isotopes and the noncarbonaceous derivation of ureilites, in common with nearly all differentiated planetary materials

Cited by 93 publications

References 93 publications

Si‐bearing metal and niningerite in Almahata Sitta fine‐grained ureilites and insights into the diversity of metal on the ureilite parent body

Si‐bearing metal and niningerite in Almahata Sitta fine‐grained ureilites and insights into the diversity of metal on the ureilite parent body

Correlated accretion ages and ε54Cr of meteorite parent bodies and the evolution of the solar nebula

Early stages of core segregation recorded by Fe isotopes in an asteroidal mantle

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Correlated accretion ages and ε⁵⁴Cr of meteorite parent bodies and the evolution of the solar nebula