V, Cr, and Mn in the Earth, Moon, EPB, and SPB and the origin of the Moon: Experimental studies

Drake, M. J.; Newsom, H. E.; Capobianco, C. J.

doi:10.1016/0016-7037(89)90328-1

Cited by 116 publications

(50 citation statements)

References 26 publications

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“…12, is 0.24 -I 0.14 for evolution between (I(Mn), €(53Cr)~) for chondrules and (I(Mn), ~(53Cr)1) for present-day Earth. This range overlaps significantly with (MdCr)Earth = 0.37 k 0.04 derivable from the Mn and Cr depletion factors for the Earth relative to CI chondrites (Drake et al, 1989), and with (Mn/Cr)Earth = 0.383 from the average of several model estimates by Birck et al (1999). Our value agrees best with values of (Mn/Cr)Earth -0.32 (Dreibus and Wanke, 1980;Hart and Zindler, 1986) at the low end of the estimates considered by Birck et al (1999).…”

Section: Evolution Of Chromium-isotopic Composition Prior To Formatiomentioning

confidence: 65%

“…It thus appears that via Mn-Cr systematics we are able to trace the evolution of the Cr-isotopic composition from condensation of the ferromagnesian precursors of chondrules to basalt generation on differentiated asteroids. As noted above, the datum for the Earth's mantle lies on or very near the isochrons for s s M n / W r = 0.42 2 0.05 (Drake et al, 1989;Anders and Grevesse, 1989); that is, the Earth appears to have the Mn-Cr systematics of a refractory (low MdCr ratio) chondrule. M d C r for the Earth, as evaluated from Fig.…”

Section: Evolution Of Chromium-isotopic Composition Prior To Formatiomentioning

confidence: 99%

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Manganese‐chromium formation intervals for chondrules from the Bishunpur and Chainpur meteorites

Nyquist

Lindstrom

Mittlefehldt

et al. 2001

Meteorit & Planetary Scien

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Abstract-Whole-chondrule Mn-Cr isochrons are presented for chondrules separated from the Chainpur (LL3.4) and Bishunpur (LL3.1) meteorites. The chondrules were initially surveyed by instrumental neutron activation analysis. LL-chondrite-normalized Mn/Cr, Mn/Fe, and Sc/Fe served to identify chondrules with unusually high or low MdCr ratios, and to correlate the abundances of other elements to Sc, the most refractory element measured. A subset of chondrules from each chondrite was chosen for analysis by a scanning electron microscope equipped with an energy dispersive x-ray spectrometer prior to high-precision Cr-isotopic analyses. 53CrPCr correlates with 55Md52Cr to give initial (53Mn/55Mn)1= (9.4 2 1.7) x 10-6 for Chainpur chondrules and (53Mn/55Mn)1= (9.5 ? 3.1) x 10-6 for Bishunpur chondrules. The corresponding chondrule formation intervals are, respectively, AtLEW = -1 0 ? 1 Ma for Chainpur and -10 k 2 Ma for Bishunpur relative to the time of igneous crystallization of the Lewis Cliff (LEW) 86010 angrite. Because MdSc correlates positively with MdCr for both the Chainpur and Bishunpur chondrules, indicating dependence of the MnlCr ratio on the relative volatility of the elements, we identify the event dated by the isochrons as volatility-driven elemental fractionation for chondrule precursors in the solar nebula. Thus, our data suggest that the precursors to LL chondrules condensed from the nebula 5.8 ? 2.7 Ma after the time when initial (53Mn/55Mn)1= (2.8 ? 0.3) x 10-5 for calcium-aluminum-rich inclusions (CAIs), our preferred value, determined from data for (a) mineral separates of type B Allende CAI BR1, (b) spinels from Efremovka CAI E38, and (c) bulk chondrites.Mn-Cr formation intervals for meteorites are presented relative to average I(Mn) = (53MdssMn)ch = 9.46 x 10-6 for chondrules. MdCr ratios for radiogenic growth of 53Cr in the solar nebula and later reservoirs are calculated relative to average (I(Mn), c(53Cr)1) = ((9.46 5 0.08) x 10-6, -0.23 k 0.08) for chondrules. Inferred values of Mn/Cr lie within expected ranges. Thus, it appears that evolution of the Cr-isotopic composition can be traced from condensation of CAIs via condensation of the ferromagnesian precursors of chondrules to basalt generation on differentiated asteroids. Measured values of ~(53Cr) for individual chondrules exhibit the entire range of values that has been observed as initial c(53Cr) values for samples from various planetary objects, and which has been attributed to radial heterogeneity in initial 53MnPMn in the early solar system. Estimated 55Md52Cr = 0.42 rt 0.05 for the bulk Earth, combined with c(53Cr) = 0 for the Earth, plots very close to the chondrule isochrons, so that the Earth appears to have the Mn-Cr systematics of a refractory chondrule. Thus, the Earth apparently formed from material that had been depleted in Mn relative to Cr contemporaneously with condensation of chondrule precursors. If, as seems likely, the Earth's core formed after complete decay of 53Mn, there must have been little differential partition...

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Section: Evolution Of Chromium-isotopic Composition Prior To Formatiomentioning

confidence: 65%

Section: Evolution Of Chromium-isotopic Composition Prior To Formatiomentioning

confidence: 99%

Manganese‐chromium formation intervals for chondrules from the Bishunpur and Chainpur meteorites

Nyquist

Lindstrom

Mittlefehldt

et al. 2001

Meteorit & Planetary Scien

View full text Add to dashboard Cite

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“…It is well known that metal-silicate partitioning of siderophile elements is a function of the oxygen fugacity (Drake et al 1989;Schmitt et al 1989). It is therefore important to estimate the f O 2 of the quenched silicate and metal liquids are, respectively, the activity, molar fraction and the activity coefficient of Fe in the metallic phase.…”

Section: (B ) Oxygen Fugacitymentioning

confidence: 99%

Partitioning experiments in the laser-heated diamond anvil cell: volatile content in the Earth's core

Jephcoat

Bouhifd

Porcelli

2008

Phil. Trans. R. Soc. A.

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The present state of the Earth evolved from energetic events that were determined early in the history of the Solar System. A key process in reconciling this state and the observable mantle composition with models of the original formation relies on understanding the planetary processing that has taken place over the past 4.5 Ga. Planetary size plays a key role and ultimately determines the pressure and temperature conditions at which the materials of the early solar nebular segregated. We summarize recent developments with the laser-heated diamond anvil cell that have made possible extension of the conventional pressure limit for partitioning experiments as well as the study of volatile trace elements. In particular, we discuss liquid-liquid, metal-silicate (M-Sil) partitioning results for several elements in a synthetic chondritic mixture, spanning a wide range of atomic number-helium to iodine. We examine the role of the core as a possible host of both siderophile and trace elements and the implications that early segregation processes at deep magma ocean conditions have for current mantle signatures, both compositional and isotopic. The results provide some of the first experimental evidence that the core is the obvious replacement for the long-sought, deep mantle reservoir. If so, they also indicate the need to understand the detailed nature and scale of core-mantle exchange processes, from atomic to macroscopic, throughout the age of the Earth to the present day.

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“…Constituent minerals in rocks from different planetary bodies are well known to have different Fe to Mn ratios (Drake et al 1989). Rocks from the earth, moon, Mars, HED parent body, and chondrites (i.e., asteroid belt) show distinct trends in Fe to Mn ratios in their mafic phases (Papike 1998).…”

Section: Lunar Originmentioning

confidence: 99%

KREEPy lunar meteorite Dhofar 287A: A new lunar mare basalt

Anand

Taylor

Misra

et al. 2003

Meteorit & Planetary Scien

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287B) is attached on the side. Dho 287A is only the fourth crystalline mare basalt meteorite found on Earth to date and is the subject of the present study. The basalt consists mainly of phenocrysts of olivine and pyroxene set in a finer-grained matrix, which is composed of elongated pyroxene and plagioclase crystals radiating from a common nucleii. The majority of olivine and pyroxene grains are zoned, from core to rim, in terms of Fe and Mg. Accessory minerals include ilmenite, chromite, ulvöspinel, troilite, and FeNi metal. Chromite is invariably mantled by ulvöspinel. This rock is unusually rich in late-stage mesostasis, composed largely of fayalite, Si-K-Ba-rich glass, fluorapatite, and whitlockite. In texture and mineralogy, Dho 287A is a low-Ti mare basalt, with similarities to Apollo 12 (A-12) and Apollo 15 (A-15) basalts. However, all plagioclase is now present as maskelynite, and its composition is atypical for known low-Ti mare basalts. The Fe to Mn ratios of olivine and pyroxene, the presence of FeNi metal, and the bulk-rock oxygen isotopic ratios, along with several other petrological features, are evidence for the lunar origin for this meteorite. Whole-rock composition further confirms the similarity of Dho 287A with A-12 and A-15 samples but requires possible KREEP assimilation to account for its rare-earth-element (REE) contents. Cooling-rate estimates, based on Fo zonation in olivine, yield values of 0.2-0.8°C/hr for the lava, typical for the center of a 10-20 m thick flow. The recalculated major-element concentrations, after removing 10-15% modal olivine, are comparable to typical A-15 mare basalts. Crystallization modeling of the recalculated Dho 287A bulk-composition yields a reasonable fit between predicted and observed mineral abundances and compositions.

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V, Cr, and Mn in the Earth, Moon, EPB, and SPB and the origin of the Moon: Experimental studies

Cited by 116 publications

References 26 publications

Manganese‐chromium formation intervals for chondrules from the Bishunpur and Chainpur meteorites

Manganese‐chromium formation intervals for chondrules from the Bishunpur and Chainpur meteorites

Partitioning experiments in the laser-heated diamond anvil cell: volatile content in the Earth's core

KREEPy lunar meteorite Dhofar 287A: A new lunar mare basalt

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