Cumberland Falls chondritic inclusions—II. Trace element contents of forsterite chondrites and meteorites of similar redox state

Verkouteren, R. Michael; Lipschutz, M. E.

doi:10.1016/0016-7037(83)90189-8

Cited by 36 publications

(18 citation statements)

References 34 publications

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“…Among three analyses of Cumberland Falls, one sample showed a high D 17 O of 0.34&; the other two samples showed usual aubritic compositions, D 17 O being À0.06& and 0.00& (Table 2). Clayton et al (1984) reported a normal aubritic oxygen isotopic composition of 0.07& in D 17 O (2.76& in d 17 O and 5.18& in d 18 O) for a bulk sample of Cumberland Falls, whereas Verkouteren and Lipschutz (1983) reported those with a high D 17 O of 0.93& for a chondritic clast in Cumberland Falls. The clast was proposed to have LL chondrite affinity based on the mineralogy and oxygen isotope compositions.…”

Section: Resultsmentioning

confidence: 92%

Noble gas and oxygen isotope studies of aubrites: A clue to origin and histories

Miura

Hidaka

Nishiizumi

et al. 2007

Geochimica et Cosmochimica Acta

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Noble gas measurements were performed for nine aubrites: Bishopville, Cumberland Falls, Mayo Belwa, Mount Egerton, Norton County, Peñ a Blanca Spring, Shallowater, ALHA 78113 and LAP 02233. These data clarify the origins and histories, particularly cosmic-ray exposure and regolith histories, of the aubrites and their parent body(ies). Accurate cosmic-ray exposure ages were obtained using the 81 Kr-Kr method for three meteorites: 52 ± 3, 49 ± 10 and 117 ± 14 Ma for Bishopville, Cumberland Falls and Mayo Belwa, respectively. Mayo Belwa shows the longest cosmic-ray exposure age determined by the 81 Kr-Kr method so far, close to the age of 121 Ma for Norton County. These are the longest ages among stony meteorites. Distribution of cosmic-ray exposure ages of aubrites implies 4-9 break-up events (except anomalous aubrites) on the parent body. Six aubrites show ''exposure at the surface'' on their parent body(ies): (i) neutron capture 36 Ar, 80 Kr, 82 Kr and/or 128 Xe probably produced on the respective parent body (Bishopville, Cumberland Falls, Mayo Belwa, Peñ a Blanca Spring, Shallowater and ALHA 78113); and/or (ii) chondritic trapped noble gases, which were likely released from chondritic inclusions preserved in the aubrite hosts (Cumberland Falls, Peñ a Blanca Spring and ALHA 78113). The concentrations of 128 Xe from neutron capture on 127 I vary among four measured specimens of Cumberland Falls (0.5-76 · 10 À14 cm 3 STP/g), but are correlated with those of radiogenic 129 Xe, implying that the concentrations of ( 128 Xe) n and ( 129 Xe) rad reflect variable abundances of iodine among specimens. The ratios of ( 128 Xe) n /( 129 Xe) rad obtained in this work are different for Mayo Belwa (0.045), Cumberland Falls (0.015) and Shallowater (0.001), meaning that neutron fluences, radiogenic 129 Xe retention ages, or both, are different among these aubrites. Shallowater contains abundant trapped Ar, Kr and Xe (2.2 · 10 À7 , 9.4 · 10 À10 and 2.8 · 10 À10 cm 3 STP/g, respectively) as reported previously (Busemann and Eugster, 2002). Isotopic compositions of Kr and Xe in Shallowater are consistent with those of Q (a primordial noble gas component trapped in chondrites). The Ar/Kr/Xe compositions are somewhat fractionated from Q, favoring lighter elements. Because of the unbrecciated nature of Shallowater, Q-like noble gases are considered to be primordial in origin. Fission Xe is found in Cumberland Falls, Mayo Belwa, Peñ a Blanca Spring, ALHA 78113 and LAP 02233. The majority of fission Xe is most likely 244 Pu-derived, and about 10-20% seems to be 238 U-derived at 136 Xe. The observed ( 136 Xe) Pu corresponds to 0.019-0.16 ppb of 244 Pu, from which the 244 Pu/U ratios are calculated as 0.002-0.009. These ratios resemble those of chondrites and other achondrites like eucrites, suggesting that no thermal resetting of the Pu-Xe system occurred after $4.5 Ga ago. We also determined oxygen isotopic compositions for four aubrites with chondritic noble gases and a new aubrite LAP 02233. In spite of their chondritic noble gas sign...

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Section: Resultsmentioning

confidence: 92%

Noble gas and oxygen isotope studies of aubrites: A clue to origin and histories

Miura

Hidaka

Nishiizumi

et al. 2007

Geochimica et Cosmochimica Acta

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“…Anyhow, following Cloutis et al (1990), enstatite is a highly transparent mineral, so a small amount of a spectrally featured material mixed in with, or adjacent to, enstatite would be detectable. For example, different aubrites such as Shallowater, Cumberland Falls, and Allan Hills 78113 contain xenoliths (composed predominantly of low iron olivine, orthopyroxene, and opaque phases (Graham et al 1977, Neal and Lipschutz 1981, Verkouteren and Lipschutz 1983, Lipschutz et al 1988) darker than the host materials, suggesting that also high albedo E-type asteroids may contain dark inclusions on their surfaces.…”

Section: Discussionmentioning

confidence: 98%

E-Type Asteroids: Spectroscopic Investigation on the 0.5μm Absorption Band

Fornasier

Lazzarin

2001

Icarus

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“…The inclusions were shocked during incorporation into the aubrite parent body (Neal and Lipschutz, 1981). We have included this material in the current paper because of the black appearance of the inclusions but note that trace element data does not match CCs (Verkouteren and Lipschutz, 1983).…”

Section: Cumberland Falls Chondritic Inclusionsmentioning

confidence: 96%

Spectral reflectance properties of carbonaceous chondrites: 8. “Other” carbonaceous chondrites: CH, ungrouped, polymict, xenolithic inclusions, and R chondrites

Cloutis

Hudon

Hiroi

et al. 2012

Icarus

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Cumberland Falls chondritic inclusions—II. Trace element contents of forsterite chondrites and meteorites of similar redox state

Cited by 36 publications

References 34 publications

Noble gas and oxygen isotope studies of aubrites: A clue to origin and histories

Noble gas and oxygen isotope studies of aubrites: A clue to origin and histories

E-Type Asteroids: Spectroscopic Investigation on the 0.5μm Absorption Band

Spectral reflectance properties of carbonaceous chondrites: 8. “Other” carbonaceous chondrites: CH, ungrouped, polymict, xenolithic inclusions, and R chondrites

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