Fractional melting and smelting on the ureilite parent body

Goodrich, C. A.; Orman, James A. Van; Wilson, Lionel

doi:10.1016/j.gca.2007.03.023

Cited by 101 publications

(178 citation statements)

References 64 publications

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“…This suggests that the highly homogeneous metal distribution in ureilites (at the meteorite scale) was determined by a post-magmatic petrogenetic process, specific to ureilites. This process may correspond to a late reduction of the olivine grain rims by reaction with carbon (Warren and Huber 2006) during cooling of the ureilites rather than the alternative model of smelting (Goodrich et al 2007) i.e., simultaneous melting and reduction by the reaction MgFeSiO 4 + C =>MgSiO 3 + Fe + CO.…”

Section: Discussionmentioning

confidence: 99%

Magnetic classification of stony meteorites: 3. Achondrites

Rochette

Gattacceca

Bourot-Denise

et al. 2009

Meteorit & Planetary Scien

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Abstract-A database of magnetic susceptibility measurements of stony achondrites (acapulcoitelodranite clan, winonaites, ureilites, angrites, aubrites, brachinites, howardite-eucrite-diogenite (HED) clan, and Martian meteorites, except lunar meteorites) is presented and compared to our previous work on chondrites. This database provides an exhaustive study of the amount of iron-nickel magnetic phases (essentially metal and more rarely pyrrhotite and titanomagnetite) in these meteorites. Except for ureilites, achondrites appear much more heterogeneous than chondrites in metal content, both at the meteorite scale and at the parent body scale. We propose a model to explain the lack of or inefficient metal segregation in a low gravity context. The relationship between grain density and magnetic susceptibility is discussed. Saturation remanence appears quite weak in most metal-bearing achondrites (HED and aubrites) compared to Martian meteorites. Ureilites are a notable exception and can carry a strong remanence, similar to most chondrites.

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Section: Discussionmentioning

confidence: 99%

Magnetic classification of stony meteorites: 3. Achondrites

Rochette

Gattacceca

Bourot-Denise

et al. 2009

Meteorit & Planetary Scien

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“…This article is a PNAS Direct Submission. 1 To whom correspondence should be addressed. Email: bischoa@uni-muenster.de.…”

Section: Significancementioning

confidence: 99%

Trachyandesitic volcanism in the early Solar System

Bischoff¹,

Horstmann²,

Barrat

et al. 2014

Proc. Natl. Acad. Sci. U.S.A.

102

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Volcanism is a substantial process during crustal growth on planetary bodies and well documented to have occurred in the early Solar System from the recognition of numerous basaltic meteorites. Considering the ureilite parent body (UPB), the compositions of magmas that formed a potential UPB crust and were complementary to the ultramafic ureilite mantle rocks are poorly constrained. Among the Almahata Sitta meteorites, a unique trachyandesite lava (with an oxygen isotope composition identical to that of common ureilites) documents the presence of volatile-and SiO 2 -rich magmas on the UPB. The magma was extracted at low degrees of disequilibrium partial melting of the UPB mantle. This trachyandesite extends the range of known ancient volcanic, crust-forming rocks and documents that volcanic rocks, similar in composition to trachyandesites on Earth, also formed on small planetary bodies ∼4.56 billion years ago. It also extends the volcanic activity on the UPB by ∼1 million years (Ma) and thus constrains the time of disruption of the body to later than 6.5 Ma after the formation of Ca-Al-rich inclusions.A large number of planetary embryos, tens to hundreds of kilometers in size, accreted within the early Solar System. In some of these embryos, internal heating triggered melting and differentiation, giving rise to a varied suite of lithologies as documented by the achondritic meteorites. Planetary crustal growth occurs via both volcanic eruptions and plutonic intrusions. Constraining these processes and the diversity of crustal materials that formed the outermost solid shell of planetary bodies is crucial for understanding Solar System planetary processes and evolution.Ureilites are among the most common achondrites and represent remnants of the mantle from a planetary body from which magmas have been extensively extracted (1−4). Several details of ureilite petrogenesis (e.g., the mode of melt extraction) remain controversial (e.g., refs. 1 and 2) because crustal rocks from the ureilite parent body (UPB) have not yet been discovered. Although tiny remnants of feldspathic and felsic melts from ureilitic breccias have been interpreted as UPB basalts or products of partial melting of plagioclase-bearing cumulates (e.g., refs. 5 and 6), it is generally assumed that the complementary melts were lost to space during explosive eruptions (e.g., refs. 7-9).A unique opportunity to gain new insights into ureilite petrogenesis was provided by the polymict asteroid 2008 TC 3 that impacted our planet October 7, 2008, in the Nubian Desert, Sudan, containing various ureilitic and ureilite-related fragments (10, 11). Among its remnant fragments collected in the strewn field, collectively named the "Almahata Sitta" meteorites, the sample ALM-A (Almahata Sitta trachyandesitic meteorite) was recovered (12). ALM-A weights 24.2 g and is covered with a greenish and shiny fusion crust (Fig. 1).The ALM-A sample described here is the only SiO 2 -rich, rapidly cooled volcanic rock among the meteorites in our collections. This rock is textura...

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“…Several previous studies have divided ureilites into different groups. For example, Goodrich et al (2004Goodrich et al ( , 2007 separated olivinepigeonite ureilites from olivine-orthopyroxene ureilites, and considered the augite-bearing lithologies to be a separate type. However, this approach cannot be applied to single mineral clasts in polymict ureilites, as it depends on information about the mineral assemblage.…”

Section: Ureilite Groupings?mentioning

confidence: 99%

“…However, the discovery of oxygen isotopic heterogeneity among ureilites (Clayton and Mayeda, 1988) made this scenario unpalatable. The current consensus is that ureilites are melt-residues of a heterogeneous parent asteroid (see discussion in Goodrich et al, 2007). Some argue that reduction by C during melting (smelting) is responsible for the range in silicate mg# of ureilites Grove, 2003, 2006;Goodrich et al, 2004).…”

Section: Models Of Evolution Of the Ureilite Parent Asteroidmentioning

confidence: 99%

“…Another distinguishing characteristic of ureilites is their extremely heterogeneous oxygen isotopic compositions that are very similar to those of the carbonaceous chondrite anhydrous mineral (CCAM) line Mayeda,1988, 1996) which may reflect heterogeneity in their chondritic precursors. The mg# heterogeneity may have been inherited from the nebula Mayeda,1988, 1996) or may have resulted from combined igneous and redox processes acting on the parent asteroid (Walker and Grove, 1993;Singletary and Grove, 2003;Goodrich et al, 2007).…”

Section: Introductionmentioning

confidence: 99%

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