Eric A. Jerde

Diamondiferous eclogites from Yakutia, Siberia: evidence for a diversity of protoliths

Major-element and REE compositions of 14 diamondiferous eclogites from the Udachnaya kimberlite in Yakutia, Siberia have been determined by electron microprobe and secondary ion mass spectrometer (SIMS). Based on previous clinopyroxene classification schemes (e.g., Taylor and Neal 1989), all of these eclogite xenoliths belong to Group B/C, although some of the garnet compositions and mineral REE abundances are inconsistent with the indicated groups. This demonstrates the inadequacy of the classification scheme based on African eclogites for application to Siberian samples. Because of the coarse grain size of the Udachnaya nodules, meaningful modal abundances could not be obtained. However, reconstructed REE compositions using various garnet: clinopyroxene ratios demonstrate relative insensitivity to changes in mode for common eclogitic assemblages. Many of these reconstructed REE compositions show LREE depletions. Some depletions are consistent with an origin (either directly or through partial melting) as “normal” or Type-I ocean floor basalt. Others, however, require material of eclogitic or pyroxenitic affinities to undergo partial melting; this facilitates the depletion of LREE while leaving the HREE at nearly original levels. Many of the eclogites of South Africa are consistent with a protolith of “anomalous” or Type II ocean floor basalt. This fundamental difference between the two regions is the likely cause of the inconsistencies with the chemicallybased classification.

Archean mantle heterogeneity and the origin of diamondiferous eclogites, Siberia; evidence from stable isotopes and hydroxyl in garnet

Abstract We have determined the phase relationships of melting of synthetic granite (two ternary feldspars + quartz) in the presence of an H2O-CO2 fluid. Synthesis and reversed experiments were conducted in a piston-cylinder apparatus over the range 650-900 °C and 6-15 kbar. At XH₂O = 0.75, melting occurred between 670 and 680 °C (15 kbar), 700 and 710 °C (10 kbar), and 710 and 720 °C (7.4 kbar). At XH₂O= 0.5, melting occurred between 760 and 770 °C (15 kbar), 780 and 790 °C (10 kbar), and 800 and 820 °C (6-7.4 kbar). At XH₂O = 0.25, melting occurred between 830 and 840 °C (15 kbar), 830 and 840 °C (10 kbar), and 860 and 870 °C (6-7.4 kbar). These results provide important constraints on the maximum temperatures of regional metamorphism attainable in vapor-saturated metapelitic and quartzofeldspathic rocks that escaped widespread melting. At pressures below 10 kbar, a fluid phase of XH₂O= 0.75, 0.5, and 0.25 limits temperatures to below ~700-725, ~800-825, and ~850-875 °C, respectively. As a consequence, the formation of granulite does not require CO2 concentrations in a coexisting fluid to exceed an XCO₂ of 0.25-0.5, a range that may include dilution of the H2O component of the fluid through internal buffering by devolatilization reactions. Therefore, the formation of granulites by the influx of CO2 may be a less common phenomenon than previously thought.

Nd and Sr isotopes from diamondiferous eclogites, Udachnaya Kimberlite Pipe, Yakutia, Siberia: Evidence of differentiation in the early Earth?

Nd and Sr isotopic data from diamond-bearing eclogites found in the Udachnaya kimberlite, Yakutia, Siberia, are interpreted as indicating an early (>1 4 Ga) differentiation event, whereby the mantle split into complementary depleted and enriched reservoirs. Reconstructed whole-rock 87Sr/S6Sr ratios (present-day) range from 0.70151 to 0.70315 and are consistent with a mantle origin for these rocks. The Nd isotopic evolution lines of four samples (U-5, U-37, U-41 and U-79) converge at 2.2-2.7 Ga. Sample U-5 is unique in exhibiting the most enriched signature of any of the samples yet analyzed (present-day end of --20), and this sample points unequivocally to an old, enriched component. A complementary depleted mantle component is suggested by two of the eclogite samples, U-86 and U-25, which yield ENd values (at 2.2 Ga) of + 13 and + 7, respectively. The two mantle reservoirs possibly formed prior to 4 Ga and evolved separately until 2.2-2.7 Ga. At that time, the reservoirs were melted forming eclogites both as residues (from the enriched reservoir) and as partial melts of peridotite (from the depleted reservoir), resulting in demonstrably different histories for eclogites from the same locality.

Exsolution of garnet within clinopyroxene of mantle eclogites: major- and trace-element chemistry

Eclogite xenoliths from the mantle have experienced a wide variety of processes and P-T conditions, many of which are recorded in the mineral compositions and textures. Exsolution of garnet from clinopyroxene is one such texture, occurring in a minority of mantle eclogites. New analyses of clinopyroxene and garnet of eclogite xenoliths from kimberlites at Bellsbank (South Africa) and Obnazhënnaya (Yakutia, Russia) are presented here, and these are combined with data from the literature. Exsolution of garnet from clinopyroxene is generally lamellar, although lens-shaped garnets are also present. Major- and trace-element characteristics show a wide range of compositions and include eclogite Groups A, B, and C. Rare-earth element (REE) concentrations of garnet and pyroxene were determined by SIMS, and the REE patterns are subtly different from those in “ordinary” eclogites. Differences include the absence of prominent Eu anomalies in samples of this study and differences in the slopes of chondrite-normalized REE patterns. It is possible that these “signatures” are unique to exsolved eclogites, a result of subsolidus elemental partitioning during exsolution. Some reconstructed whole-rock compositions are aluminuous; comparison with ordinary eclogites shows only minor differences, implying a similar origin. If the immediate precursor to the exsolved eclogites was a monomineralic pyroxenite, the excess aluminium was tied up in Tschermaks molecule, although the occasional presence of kyanite exsolution lamellae is indicative of a Ca-Eskola component. Reconstructed “pyroxenes” from kyanite- and corundum-rich samples contain unrealistic amounts of aluminium for mantle pyroxenes. A protolith (or parental pyroxene) “threshold” of ∼24% Al2O3 may exist, above which (as in a plagioclase cumulate) the final assemblage is kyanite- and/or corundum-bearing.

Evolution of the upper mantle of the Earth's Moon: Neodymium and strontium isotopic constraints from high-Ti mare basalts

Isotopic studies of mare basalts have led workers to conclude that their sources are heterogeneous on both large and small scales. Furthermore, these studies have led workers to postulate that depletion within the lunar mantle occurred early in its evolution and was a result of accumulation of mafic minerals from a LREE-enriched magma ocean. High-Ti basalts from the Apollo 1 I and 17 landing sites and ilmenite basalts from Apollo 12 are secondary evidence of this extreme, early depletion event. KREEPy rocks are the complementary enriched component in the Moon. A total of fourteen high-Ti basalts have now been analyzed from the Apollo 11 landing site for neo- dymium and strontium isotopes. A Sm-Nd internal isochron on basalt 10058 yields an age of 3.70 + 0.06 Ga, similar to 40Ar/39Ar ages of other Group B 1 basal@.. A compilation of all previously determined ages on Apollo 11 high-Ti basalts indicates four distinct phases of volcanism at 3.85 + 0.02 Ga (Group B2), 3.71 f 0.02 Ga (Group B3), 3.67 + 0.02 Ga (Group Bl), and 3.59 f 0.04 Ga (Group A). Whole- rock Sm-Nd isotopic data for all Apollo 11 high-Ti basalts form a linear array, which yields the age of the Moon (4.55 f 0.30 Ga). A similar regression of all uncontaminated high-Ti basalts from the Moon (both Apollo 11 and Apollo 17) yields an age of 4.46 + 0.17 Ga. Both arrays are interpreted as average source ages of the high-Ti basalts and are consistent with the formation of these sources by precipitation of cumulates from a magma ocean early in the history of the Moon. These new strontium and neodymium isotopic data, coupled with previously published data, are con- sistent with a two-component model for the upper mantle of the Moon. These two components include mafic adcumulates precipitated from a magma ocean prior to 4.4 Ga and small amounts (~2%) of trapped, KREEPy, late-stage, magma ocean differentiates. The mafic adcumulate evolves from 4.5 Ga, with 47Sm/44Nd = 0.318 and *Rb/%r = 0.005 to extremely radiogenic neodymium isotopic ratios and very unradiogenic strontium isotopic ratios. The KREEPy trapped liquid has a 14Sm/ 44Nd = 0.168 and Rb/%r = 0.235 and thus, evolves toward very unradiogenic neodymium and radiogenic strontium isotopic ratios. Because the KREEPy trapped liquid is enriched in both rubidium and the REEs by over an order of magnitude compared to the mafic adcumulate, trapping of even small proportions of this liquid in the adcumulate will control the radiogenic isotopic composition of the source. The apparent heterogeneity in the source regions of mare basalts could be caused by trapping of variable, yet small, proportions of this LILE-enriched liquid in the cumulate pile.

The origin and evolution of lunar high-Ti basalts: Periodic melting of a single source at Mare Tranquillitatis

Abstract Five groups of basalts (A, B1, B2, B3, D) with three principal ages exist at the Apollo 11 site. These range from the low-K, low rare-earth element (REE) Groups B1, B2, and B3 to the low-K, high REE Group D basalts, to the high-K, high-REE Group A basalts. The Group A basalts are the only high-K (>0.2 wt% K2O) basalts, and youngest, with an age of 3.59 ± .02 Ga; Groups B3 and B1 are 3.71 ± .02 and 3.67 ± .02 Ga, respectively; Group B2 basalts are the oldest, at 3.85 ± .02 Ga. Group D basalts have not been dated. Fractionation modelling for major and trace elements indicates that the B1 basalts could have formed from a B3-like parent liquid. The B2 and D basalts can also be related to liquids similar to the B3-B1 composition through the presence of varying amounts of modal whitlockite. Thus, the entirety of low-K high-Ti basalts at Apollo 11 may have formed through melting of the same source region. The Group A basalt compositions are consistent with formation from a different parent liquid, with the composition of Apollo 11 orange glass. Modelling of major- and trace-elements in the Apollo 11 orange glass, indicate that the composition of the Group A basalts is consistent with fractionation of this glass, coupled with some assimilation (~7.5–15%) of an evolved KREEP-like material. However, this component is much younger than primitive KREEP (4.4 Ga). This “neuKREEP” component, similar to the composition of quartz monzodiorites described from the Apollo 15 site, probably represents evolved material formed during plutonism prior to the formation of the Apollo 11 orange glass liquid.

Petrogenesis of Garnet Pyroxenite and Spinel Peridotite Xenoliths of the Tell-Danun Alkali Basalt Volcano, Harrat As Shamah, Syria

A suite of samples, including kaersutite and ilmenite megacrysts, spinel peridotites, garnet pyroxenites, and the alkali basalts that host them, have been studied in an effort to better constrain the mineralogy and chemistry of the subcontinental mantle beneath the central portion of the Arabian plate. Kaersutite megacrysts are classified as Type-A high-pressure precipitates of the alkali basalt host, which transported these xenoliths to the surface and extruded them during formation of the Tell-Danun volcano, southwestern Syria. Ilmenite megacrysts are classified as Type-B megacrysts and could not have precipitated from the alkali basalts presently sampled. Instead, they were derived from a magma that was enriched in the rare-earth elements (REE) by ca. four times and depleted in Zr and Hf, compared to the alkali basalts. Garnet pyroxenites from the Tell-Danun volcanic field yield temperatures and pressures of 946-1045° C and 8-10 kbar, respectively. These xenoliths likely were precipitated as dikes or a...

Petrology and Chemistry of an Early Proterozoic Lherzolite-Gabbronorite-Anorthosite Pluton of the White Sea Complex, Northern Karelia, Russia

Two of the most well-preserved igneous bodies in the early Preeambrian White Sea complex— the Severnyy and Yuzhnyy massifs on Pezhostrov Island—have been studied in order to gain a better understanding of ultramafic-mafic magmatism in the Belomorian tectonic block. These massifs represent portions of a single, differentiated pluton, ranging in composition from lherzolite to gabbronorite to anorthosite. Mineral-chemical and trace-element compositions of chill margins from this pluton were used to model the differentiation in this ancient magma chamber. Major-element compositions of minerals suggest that plagioclase in these rocks is not in equilibrium with the mafic minerals. This possibly is the result of suspension of less dense, early-formed plagioclase in more dense, early residual liquids. Later, as the liquid density decreased because of precipitation of mafic phases, plagioclase began to precipitate. We speculate that the liquid density did not decrease to a point where plagioclase would settle, unt...