The differentiation of eucrites: The role of <i>in situ</i> crystallization

Barrat, Jean‐Alix; Blichert‐Toft, Janne; Gillet, Ph.; Keller, Francine

doi:10.1111/j.1945-5100.2000.tb01495.x

Cited by 112 publications

(150 citation statements)

References 54 publications

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“…As observed in most of the known eucrites, there are no systematic differences in chemical compositions of minerals among different textural regions. The chemical data are broadly consistent with literature values for noncumulate eucrites, although TiO 2 values are lower than those presented by Barrat et al (2000) (Figure 8). …”

Section: Discussionsupporting

confidence: 80%

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Serra Pelada: the first Amazonian Meteorite fall is a Eucrite (basalt) from Asteroid 4-Vesta

Zucolotto

Tosi

Villaça

et al. 2018

An. Acad. Bras. Ciênc.

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Serra Pelada is the newest Brazilian eucrite and the first recovered fall from Amazonia (State of Pará, Brazil, June 29 th 2017). In this paper, we report on its petrography, chemistry, mineralogy and its magnetic properties. Study of four thin sections reveals that the meteorite is brecciated, containing basaltic and gabbroic clasts, as well of recrystallized impact melt, embedded into a fine-medium grained matrix. Chemical analyses suggest that Serra Pelada is a monomict basaltic eucritic breccia, and that the meteorite is a normal member of the HED suite. Our results provide additional geological and compositional information on the lithological diversity of its parent body. The mineralogy of Serra Pelada consists basically of low-Ca pyroxene and high-Ca plagioclase with accessory minerals such as quartz, sulphide (troilite), chromite -ulvöspinel and ilmenite. These data are consistent with the meteorite being an eucrite, a basaltic achondrite and a member of the howardite-eucrite-diogenite (HED) clan of meteorites which most likely are from the crust asteroid 4 Vesta.Key words: Serra Pelada, meteorite, eucrite, Vesta, Brazilian Meteorite.

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Section: Discussionsupporting

confidence: 80%

“…Comparing the percentage of TiO 2 and FeO/MgO ratio of Serra Pelada with the literature (Figure 8), the Serra Pelada FeO/MgO ratio is located in the region close to that of noncumulate eucrites (Barrat et al 2000), although the TiO 2 wt% is lower than expected for these meteorites.…”

Section: Discussionmentioning

confidence: 96%

Serra Pelada: the first Amazonian Meteorite fall is a Eucrite (basalt) from Asteroid 4-Vesta

Zucolotto

Tosi

Villaça

et al. 2018

An. Acad. Bras. Ciênc.

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“…In addition, three modern island arc basalts (IABs) from New Britain (NMNH 116852-1, 116852-3 and 116852-11) were also analyzed here to test the accuracy of the measurements (see Dauphas et al (2009a) for a detailed discussion about IABs). (Jarosewich, 1990); NWA1950 (Gillet et al, 2005); Los Angeles (Warren et al, 2000); EETA79001, ALHA77005, Nakhla, ALH84001 (Lodders, 1998); Mil03346 (Day et al, 2006); GRO95555, MET00436, MET00424 ; NWA1461 (Warren et al, 2009);Shalka (McCarthy et al, 1972); ALHA77256 (Sack et al, 1991); NWA1240, NWA049 (Barrat et al, 2003); Cachari (Barrat et al, 2000); Agoult, Dag945 (Yamaguchi et al, 2009); Nuevo Laredo, NWA4523 (Barrat et al, 2007b); D'Orbigny, Sahara99555 (Mittlefehldt et al, 2002);LEW86010 (McKay et al, 1988); NWA1670 (Jambon et al, 2008); NWA1296 (Jambon et al, 2005); NWA2999 (Gellissen et al, 2007). i Weathering conditions are from MetBase (version 7.1).…”

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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“…The study of HED cumulate lithologies provides a complementary view of early magmatic processes on Vesta. Although it is generally accepted that a few gabbros, the cumulate eucrites, formed from "ordinary" eucritic melts (Treiman 1997;Barrat et al 2000a;Saiki et al 2001;Barrat 2004), the origin of the diogenites and the composition of their parental melts remain unresolved (e.g., Mittlefehldt 1994;Fowler et al 1994Fowler et al , 1995Shearer et al 1997;Barrat 2004). Diogenites are believed to be a major lithological component of Vesta.…”

Section: Introductionmentioning

confidence: 99%

Geochemistry of diogenites: Still more diversity in their parental melts

Barrat

Yamaguchi

Greenwood

et al. 2008

Meteorit & Planetary Scien

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100

154

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Abstract-We report on the major and trace element abundances of 18 diogenites, and O-isotopes for 3 of them. Our analyses extend significantly the diogenite compositional range, both in respect of Mg-rich (e.g., Meteorite Hills [MET] 00425, MgO = 31.5 wt%) and Mg-poor varieties (e.g., Dhofar 700, MgO = 23 wt%). The wide ranges of siderophile and chalcophile element abundances are well explained by the presence of inhomogeneously distributed sulfide or metal grains within the analyzed chips. The behavior of incompatible elements in diogenites is more complex, as exemplified by the diversity of their REE patterns. Apart from a few diogenite samples that contain minute amounts of phosphate, and whose incompatible element abundances are unlike the orthopyroxene ones, the range of incompatible element abundances, and particularly the range of Dy/Yb ratios in diogenites is best explained by the diversity of their parental melts. We estimate that the FeO/MgO ratios of the diogenite parental melts range from about 1.4 to 3.5 and therefore largely overlap the values obtained for non-cumulate eucrites. Our results rule out the often accepted view that all the diogenites formed from parental melts more primitive than eucrites during the crystallization of a magma ocean. Instead, they point to a more complex history, and suggest that diogenites were derived from liquids produced by the remelting of cumulates formed from the magma ocean.

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The differentiation of eucrites: The role of in situ crystallization

Cited by 112 publications

References 54 publications

Serra Pelada: the first Amazonian Meteorite fall is a Eucrite (basalt) from Asteroid 4-Vesta

Serra Pelada: the first Amazonian Meteorite fall is a Eucrite (basalt) from Asteroid 4-Vesta

Iron isotope fractionation in planetary crusts

Geochemistry of diogenites: Still more diversity in their parental melts

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