Petrogenesis of picritic mare magmas: Constraints on the extent of early lunar differentiation

Calculations of isobaric batch, polybaric batch, and polybaric fractional melting have been carried out on a variety of proposed lunar and terrestrial source region compositions. Results show that magmas with a generally tholeiitic character—plagioclase and high-Ca pyroxene crystallize before low-Ca pyroxene reflecting relatively high Al₂O₃ concentrations (>12 wt%)—are the inevitable consequence of anhydrous partial melting of source regions composed primarily of olivine and two pyroxenes with an aluminous phase on the solidus. Low-Al₂O₃ magmas (<10 wt%), as typified by the green picritic glasses in the lunar maria require deep (700–1000 km), low-Al₂O₃ source regions without an aluminous phase. The difference between primitive and depleted mantle beneath mid-ocean ridges amounts to less than 0.1 wt% Al₂O₃, whereas formation of the green glass source region requires a net loss of between 1.5 and 2.5 wt% Al₂O₃. Basalt extraction cannot account for fractionations of this magnitude. Accumulation of olivine and pyroxene at the base of a crystallizing magma ocean is, however, an effective method for producing the necessary Al₂O₃ depletions. Both olivine-rich and pyroxene-rich source regions can produce the picritic magmas, but mixing calculations show that both types of source region are likely to be hybrids consisting of an early- to intermediate-stage cumulate (olivine plus enstatite) and a later stage cumulate assemblage. Mass balance calculations show that refractory element-enriched bulk Moon compositions contain too much Al₂O₃ to allow for the deep low-Al₂O₃ source regions even after extraction of an Al₂O₃-rich (26–30 wt%) crust between 50 and 70 km thick.     

The origin of organic matter in the solar system: evidence from the interplanetary dust particles

The detailed examination of meteorites and interplanetary dust particles provides an opportunity to infer the origin of the organic matter found in primitive Solar System materials. If this organic matter were produced by aqueous alteration of elemental (graphitic or amorphous) carbon on an asteroid, then we would expect to see the organic matter occurring preferentially in interplanetary materials that exhibit evidence of aqueous activity, such as the presence of hydrated silicates. On the other hand, if the organic matter were produced either during the nebula phase of Solar System evolution or in the interstellar medium, we might expect this organic matter to be incorporated into the dust as it formed. In that case pre-biotic organic matter would be present in both the anhydrous and the hydrated interplanetary materials. We have performed carbon X-ray absorption near-edge structure spectroscopy and infrared spectroscopy on primitive anhydrous and hydrated interplanetary dust particles (IDPs) collected by NASA from the Earth's stratosphere. We find that organic matter is present in similar types and abundances in both the anhydrous and the hydrated IDPs, and, in the anhydrous IDPs some of this organic matter is the “glue” that holds grains together. These measurements provide the first direct, experimental evidence from the comparison of extraterrestrial samples that the bulk of the pre-biotic organic matter occurs in similar types and abundances in both hydrated and anhydrous samples. This indicates that the bulk of the pre-biotic organic matter in the Solar System did not form by aqueous processing, but, instead, had already formed at the time that primitive, anhydrous dust was being assembled. Thus, the bulk of the pre-biotic organic matter in the Solar System was formed by non-aqueous processing, occurring in either the Solar nebula or in an interstellar environment. Aqueous processing on asteroids may have altered this pre-existing organic matter, but such processing did not affect in any substantial way the C=O content of the organic matter, the aliphatic C-H abundance, or the mean aliphatic chain length.     

Large-scale silicate liquid immiscibility: a possible example from northeastern Brazil

Ultrapotassic, peralkalic silica-saturated plutons (580 Ma) are widespread in the Cachoeirinha-Salgueiro foldbelt, northeastern Brazil. They consist of alkali-feldspar syenites with pyroxenite as co-magmatic inclusions and syn-plutonic or late-stage dikes. Pyroxenite and syenite have the same mineral phases (aegirine-augite, microcline, sphene, apatite, blue amphibole, magnetite), but only in different proportions. Rare inclusions of a “mixed” rock (about 60% syenite+40% pyroxenite in an emulsion-like texture) are also present. Pyroxenes in the three units are all only slightly zoned, silica-saturated and extremely low in Al₂O₃ (0.2–1.4%). Amphiboles are mostly K-rich richterite, characterized by high SiO₂, low Al₂O₃ and TiO₂ contents and low Mg#.

The three rock types have similar REE chondrite-normalized patterns, with negative slopes and lack of Eu anomaly, with the total REE in the pyroxenite greater than that of the syenite. Trace element patterns for the mixed rock are intermediate between those for the pyroxenite and syenite. Major element partitioning between pyroxenite and syenite has the same sense as that one observed between immiscible liquids in volcanic lavas and trace element partitioning is similar to the experimentally determined partition of immiscible liquid pairs.

The rocks have similar high δ¹⁸O values (avg. w.r.+ 8‰_SMOW, corrected from pyroxene), high initial ⁸⁷Sr/⁸⁶Sr ratios (about 0.710), and low ¹⁴³Nd/¹⁴⁴Nd (avg. 0.51104).

Field and geochemical characteristics indicate chemical equilibrium among the three rock types and suggest liquid immiscibility between syenite and pyroxenite, the mixed rock representing the original magma composition.     

Identification of isotopically primitive interplanetary dust particles: A NanoSIMS isotopic imaging study

We have carried out a comprehensive survey of the isotopic compositions (H, B, C, N, O, and S) of a suite of interplanetary dust particles (IDPs), including both cluster and individual particles. Isotopic imaging with the NanoSIMS shows the presence of numerous discrete hotspots that are strongly enriched in ¹⁵N, up to ∼1300‰. A number of the IDPs also contain larger regions with more modest enrichments in ¹⁵N, leading to average bulk N isotopic compositions that are ¹⁵N-enriched in these IDPs. Although C isotopic compositions are normal in most of the IDPs, two ¹⁵N-rich hotspots have correlated ¹³C anomalies. CN⁻/C⁻ ratios suggest that most of the ¹⁵N-rich hotspots are associated with relatively N-poor carbonaceous matter, although specific carriers have not been determined. H isotopic distributions are similar to those of N: D anomalies are present both as distinct D-rich hotspots and as larger regions with more modest enrichments. Nevertheless, H and N isotopic anomalies are not directly correlated, consistent with results from previous studies. Oxygen isotopic imaging shows the presence of abundant presolar silicate grains in some of the IDPs. The O isotopic compositions of the grains are similar to those of presolar oxide and silicate grains from primitive meteorites. Most of the silicate grains in the IDPs have isotopic ratios consistent with meteoritic Group 1 oxide grains, indicating origins in oxygen-rich red giant and asymptotic giant branch stars, but several presolar silicates exhibit the ¹⁷O and ¹⁸O enrichments of Group 4 oxide grains, whose origin is less well understood. Based on their N isotopic compositions, the IDPs studied here can be divided into two groups. One group is characterized as being “isotopically primitive” and consists of those IDPs that have anomalous bulk N isotopic compositions. These particles typically also contain numerous ¹⁵N-rich hotspots, occasional C isotopic anomalies, and abundant presolar silicate grains. In contrast, the other “isotopically normal” IDPs have normal bulk N isotopic compositions and, although some contain ¹⁵N-rich hotspots, none exhibit C isotopic anomalies and none contain presolar silicate or oxide grains. Thus, isotopically interesting IDPs can be identified and selected on the basis of their bulk N isotopic compositions for further study. However, this distinction does not appear to extend to H isotopic compositions. Although both H and N anomalies are frequently attributed to the survival of molecular cloud material in IDPs and, thus, should be more common in IDPs with anomalous bulk N compositions, D anomalies are as common in normal IDPs as they are in those characterized as isotopically primitive, based on their N isotopes.     

准噶尔盆地玛湖凹陷下二叠统风城组含碱层段韵律特征及成因*

准噶尔盆地玛湖凹陷早二叠世风城组沉积时期为典型的碳酸盐型咸化湖盆,湖盆咸化过程中析出大量的碱矿(钠碳酸盐类矿物)。通过含碱层段主量元素、碳氧同位素分析,结合岩心宏观及微观矿物岩石特征,探讨了含碱层段韵律特征及形成机理。研究层段碱矿与沉凝灰岩互层,形成明暗相间的咸化韵律。浅色碱矿层质地较纯,主要为苏打和小苏打,主量元素表现为 Na₂O含量高,CaO、MgO、SiO₂和Al₂O₃含量低;暗色层段主要为含斑点状碳钠钙石的沉凝灰岩,主量元素表现为Na₂O含量低,CaO、MgO、SiO₂和Al₂O₃含量高。浅色碱矿层和暗色沉凝灰岩段碳氧同位素值均为正,表明其沉积水体具高盐度特征。浅色含碱层段具有更高的 δ¹⁸O 值,反映了碱矿层沉积时期强烈蒸发的气候条件。根据δ¹⁸O/δ¹³C值的波动将研究层段划分为炎热干旱和相对湿润的气候条件,并据此解释不同韵律层盐类矿物形成机理。暗色的沉凝灰岩沉积代表地表流水注入量大于蒸发量,沉凝灰岩中盐类矿物含量少或者呈斑点状从颗粒间的卤水中析出;随着蒸发量的增高以及古气候由温暖潮湿转变为干旱炎热,地表流水注入量急剧减少,强烈蒸发控制了碱矿的沉积,形成浅色质地较纯的碱矿层。气候的频繁交替形成了风二段碱矿与沉凝灰岩频繁互层的特征。     

Lunar geochemistry as told by lunar meteorites

About 36 lunar meteorites have been found in cold and hot deserts since the first one was found in 1979 in Antarctica. All are random samples ejected from unknown locations on the Moon by meteoroid impacts. Lithologically and compositionally there are three extreme types: (1) brecciated anorthosites with high Al₂O₃ (26–31%), low FeO (3–6%), and low incompatible elements (e.g., <1 μg/g Th), (2) basalts and brecciated basalts with high FeO (18–22%), moderately low Al₂O₃ (8–10%) and incompatible elements (0.4–2.1 μg/g Th), and (3) an impact-melt breccia of noritic composition (16% Al₂O₃, 11% FeO) with very high concentrations of incompatible elements (33 μg/g Th), a lithology that is identified as KREEP on the basis of its similarity to Apollo samples of that designation. Several meteorites are polymict breccias of intermediate composition because they contain both anorthosite and basalt. Despite the large range in compositions, a variety of compositional parameters together distinguish lunar meteorites from terrestrial materials. Compositional and petrographic data for lunar meteorites, when combined with mineralogical and compositional data obtained from orbiting spacecraft in the 1990s, suggest that Apollo samples identified with the magnesian (Mg-rich) suite of nonmare rocks (norite, troctolite, dunite, alkali anorthosite, and KREEP) are all products of a small, geochemically anomalous (noritic, high Th) region of crust known as the Procellarum KREEP Terrane and are not, as generally assumed, indigenous to the vast expanse of typical feldspathic crust known as the Feldspathic Highlands Terrane. Magnesian-suite rocks such as those of the Apollo collection do not occur as clasts in the feldspathic lunar meteorites. The misconception is a consequence of four historical factors: (1) the Moon has long been viewed as simply bimodal in geology, mare or highlands, (2) one of the last, large basin-forming bolides impacted in the Procellarum KREEP Terrane, dispersing Th-rich material, (3) although it was not known at the time, the Apollo missions all landed in or near the anomalous Procellarum KREEP Terrane and collected many Th-rich samples formed therein, and (4) the Apollo samples were interpreted and models for lunar crust formation developed without recognition of the anomaly because global data provided by orbiting missions and lunar meteorites were obtained only years later.     

Auger Nanoprobe analysis of presolar ferromagnesian silicate grains from primitive CR chondrites QUE 99177 and MET 00426

We have investigated the presolar grain inventories of two CR chondrites, QUE 99177 and MET 00426, which are less altered than most members of this meteorite group. Both meteorites contain high abundances of O-anomalous presolar grains, with concentrations of 220 ± 40 and 160 ± 30 ppm for QUE 99177 and MET 00426, respectively. The presolar grain inventories are dominated by ferromagnesian silicates with group 1 oxygen isotopic compositions, indicative of origins in low mass red giant or asymptotic giant branch stars. Grains with pyroxene-like compositions are somewhat more common than those with olivine-like compositions, but most grains are non-stoichiometric with compositions intermediate between these two phases, consistent with recent work suggesting that amorphous interstellar silicates have stoichiometries between olivine and pyroxene type silicates. Although structural data are not available, one grain contains only Si and O, and has a stoichiometry consistent with SiO₂.Our presolar grains are much more Fe-rich than predicted by astronomical observations. Although secondary alteration may play a role in enhancing the Fe contents of presolar grains, it seems unlikely that the large and ubiquitous Fe enrichments observed in the grains from this study can be due only to secondary processing, particularly given the highly primitive nature of these two meteorites. Grain condensation in the stellar outflows where these grains formed likely proceeded under rapidly changing kinetic conditions that may have enhanced the incorporation of Fe into the grains over that expected based on equilibrium condensation theory.Both QUE 99177 and MET 00426 appear to contain unusually low abundances of oxide grains and have higher silicate/oxide ratios than other primitive meteorites analyzed to date. We explore various possibilities for this discrepancy, but note that most scenarios are not likely to result in the preferential destruction of oxides relative to silicates. Thus, the highest silicate/oxide ratios, such as those observed in the CR chondrites, should reflect the true initial proportions of presolar silicate and oxide grains in the parent molecular cloud from which the solar nebula evolved.     

陇东新近纪红粘土与第四纪黄土地球化学特征及其物源和风化指示意义

甘肃省平凉市灵台县邵寨镇剖面风尘堆积底界年龄大约为5.23 Ma B.P.,通过对该剖面新近纪红粘土与第四纪黄土-古土壤序列的常量元素、 微量元素、Nd同位素的测试,分析其在物源和风化方面的指示意义,发现新近纪红粘土与第四纪黄土具有相似的常量、 微量元素UCC标准化曲线和稀土元素球粒陨石标准化曲线,指示二者皆来自广阔的...     

Oxygen isotopic composition of minerals in the Kenna ureilite

The δ¹⁸O and δ¹⁷O values of olivine from Kenna are 7.6 and 3.0%, respectively, relative to SMOW. These values are typical of ureilites which form a unique group on a δ¹⁷O -δ¹⁸O graph. The ureilites are related to, but not directly derived from, the anhydrous phases of C2 and C3 meteorites. The ¹⁸O/¹⁶O fractionation between pyroxene and olivine is 0.60, indicating a temperature of last equilibration of 1000 ± 100°C.     

重庆高燕地区菱锰矿热水沉积成因地球化学证据

重庆高燕锰矿床位于晚震旦世秦巴成锰沉积盆地,主要赋存于陡山沱组顶部,以鲕粒或球粒状产出.为了查明其成因,在收集该区锰矿相关成果的基础上,对ZK129-3^#、ZK115-7^#、ZK127-7^#、ZK133-7^#、ZK115-11^#五个钻孔的陡山沱组鲕状菱锰矿进行系统采样,并测试了包括Mn、Fe、P、SiO₂、CaO、MgO、Al₂O₃和LOI在内的8个地球化学指标,进而运用指相元素地球化学分析了Mn/Al、（MgO/Al₂O₃）×10²、Al/（Al+Fe+Mn）和SiO₂/Al₂O₃比值.结果表明：重庆高燕菱锰矿受陆源物质的影响很小,与海洋沉积有关,主要是海洋自生产物;Al/（Al+Fe+Mn）和SiO₂/Al₂O₃值则指示其沉积过程中有热水参与,是热水沉积的产物.     

Oxidized, magnetite-series, rapakivi-type granites of Carajás, Brazil: Implications for classification and petrogenesis of A-type granites

The varying geochemical and petrogenetic nature of A-type granites is a controversial issue. The oxidized, magnetite-series A-type granites, defined by Anderson and Bender [Anderson, J.L., Bender, E.E., 1989. Nature and origin of Proterozoic A-type granitic magmatism in the southwestern United States of America. Lithos 23, 19–52.], are the most problematic as they do not strictly follow the original definition of A-type granites, and approach calc-alkaline and I-type granites in some aspects. The oxidized Jamon suite A-type granites of the Carajás province of the Amazonian craton are compared with the magnetite-series granites of Laurentia, and other representative A-type granites, including Finnish rapakivi and Lachlan Fold Belt A-type granites, as well as with calc-alkaline, I-type orogenic granites. The geochemistry and petrogenesis of different groups of A-types granites are discussed with an emphasis on oxidized A-type granites in order to define their geochemical signatures and to clarify the processes involved in their petrogenesis. Oxidized A-type granites are clearly distinguished from calc-alkaline Cordilleran granites not only regarding trace element composition, as previously demonstrated, but also in their major element geochemistry. Oxidized A-type granites have high whole-rock FeO_t/(FeO_t + MgO), TiO₂/MgO, and K₂O/Na₂O and low Al₂O₃ and CaO compared to calc-alkaline granites. The contrast of Al₂O₃ contents in these two granite groups is remarkable. The CaO/(FeO_t + MgO + TiO₂) vs. CaO + Al₂O₃ and CaO/(FeO_t + MgO + TiO₂) vs. Al₂O₃ diagrams are proposed to distinguish A-type and calc-alkaline granites. Whole-rock FeO_t/(FeO_t + MgO) and the FeO_t/(FeO_t + MgO) vs. Al₂O₃ and FeO_t/(FeO_t + MgO) vs. Al₂O₃/(K₂O/Na₂O) diagrams are suggested for discrimination of oxidized and reduced A-type granites. Experimental data indicate that, besides pressure, the nature of A-type granites is dependent of ƒO₂ conditions and the water content of magma sources. Oxidized A-type magmas are considered to be derived from melts with appreciable water contents (≥ 4 wt.%), originating from lower crustal quartz-feldspathic igneous sources under oxidizing conditions, and which had clinopyroxene as an important residual phase. Reduced A-type granites may be derived from quartz-feldspathic igneous sources with a metasedimentary component or, alternatively, from differentiated tholeiitic sources. The imprint of the different magma sources is largely responsible for the geochemical and petrological contrasts between distinct A-type granite groups. Assuming conditions near the NNO buffer as a minimum for oxidized granites, magnetite-bearing granites formed near FMQ buffer conditions are not stricto sensu oxidized granites and a correspondence between oxidized and reduced A-type granites and, respectively, magnetite-series and ilmenite-series granites is not always observed.     

The origin of medium-K ankaramitic arc magmas from Lombok (Sunda arc, Indonesia): Mineral and melt inclusion evidence

High-calcium, nepheline-normative ankaramitic basalts (MgO > 10 wt.%, CaO/Al₂O₃ > 1) from Rinjani volcano, Lombok (Sunda arc, Indonesia) contain phenocrysts of clinopyroxene and olivine (Fo_85–92) with inclusions of spinel (Cr# 58–77) and crystallised melt. Olivine crystals have variable but on average low NiO (0.10–0.23 wt.%) and high CaO (0.22–0.35 wt.%) contents for their forsterite number. The CaO content of Fo_89–91 olivine is negatively correlated with the Al₂O₃ content of enclosed spinel (9–15 wt.%) and positively correlated with the CaO/Al₂O₃ ratios of melt inclusions (0.9–1.5). Major and trace element patterns of melt inclusions are similar to that of the host rock, indicating that the magma could have formed by accumulation of small batches of melt, with compositions similar to the melt inclusions. The liquidus temperature of the magma was  1275 °C, and its oxygen fugacity ≤ FMQ + 2.5. Correlations between K₂O, Zr, Th and LREE in the melt inclusions are interpreted to reflect variable degrees of melting of the source; correlations between Al₂O₃, Na₂O, Y and HREE are influenced by variations in the mineralogy of the source. The melts probably formed from a water-poor, clinopyroxene-rich mantle source.     

The nature of molecular cloud material in interplanetary dust

Eight interplanetary dust particles (IDPs) exhibiting a wide range of H and N isotopic anomalies have been studied by transmission electron microscopy, x-ray absorption near-edge structure spectroscopy, and Fourier-transform infrared spectroscopy. These anomalies are believed to have originated during chemical reactions in a cold molecular cloud that was the precursor to the Solar System. The chemical and mineralogical studies reported here thus constitute direct studies of preserved molecular cloud materials. The H and N isotopic anomalies are hosted by different hydrocarbons that reside in the abundant carbonaceous matrix of the IDPs. Infrared measurements constrain the major deuterium (D) host in the D-enriched IDPs to thermally labile aliphatic hydrocarbon groups attached to macromolecular material. Much of the large variation observed in D/H in this suite of IDPs reflects the variable loss of this labile component during atmospheric entry heating. IDPs with elevated ¹⁵N/¹⁴N ratios contain N in the form of amine (-NH₂) functional groups that are likely attached to other molecules such as aromatic hydrocarbons. The host of the N isotopic anomalies is not as readily lost during entry heating as the D-rich material. Infrared analysis shows that while the organic matter in primitive anhydrous IDPs is similar to that observed in acid residues of primitive chondritic meteorites, the measured aromatic:aliphatic ratio is markedly lower in the IDPs.     

The nature of the sub-continental mantle: constraints from the major-element composition of continental flood basalts

Many continental flood basalts (CFB) have isotope and trace-element signatures that differ from those of oceanic basalts and much interest concerns the extent to which these reflect differences in their upper mantle source regions. A review of selected data sets from the Mesozoic and Tertiary CFB confirms significant differences in their major- and trace-element compositions compared with those of basalts erupted through oceanic lithosphere. In general, those CFB suites characterised by low Nb/La, high (⁸⁷Sr/⁸⁶Sr)_i and low εNd_i tend to exhibit relatively low TiO₂, CaO/Al₂O₃, Na₂O and/or Fe₂O₃, and relatively high SiO₂. In contrast, those which have high Nb/La, low (⁸⁷Sr/⁸⁶Sr)_i and high εNd_i ratios, like the upper units in the Deccan Traps, have major- and trace-element compositions similar to oceanic basalts. It would appear that those CFB that have distinctive isotope and trace-element ratios also exhibit distinctive major-element contents, suggesting that major and trace elements have not been decoupled significantly during magma generation and differentiation.

When compared (at 8% MgO) with oceanic basalt trends, the displacement of many CFB to lower Na₂O, Fe₂O₃^*, TiO₂ and CaO/Al₂O₃, but higher SiO₂, at similar Mg#, is not readily explicable by crustal contamination. Rather, it reflects source composition and/or the effects of the melting processes. The model compositions of melts produced by decompression of mantle plumes beneath continental lithosphere have relatively low SiO₂ and high Fe₂O₃^*. In contrast, the available experimental data indicate that partial melts of peridotite have low TiO₂, Na₂O and Fe₂O₃^*CaO/Al₂O₃, if the peridotite has been previously depleted by melt extraction. Moreover, melting of hydrated, depleted peridotite yields SiO₂-rich, Fe₂O₃- and CaO-poor melts. Since anhydrous, depleted peridotite has a high-temperature solidus, it is argued that the source of these CFB was variably melt depleted and hydrated mantle, inferred to be within the lithosphere. Isotope data suggest these source regions were often old and relatively enriched in incompatible trace elements, and it is envisaged that H₂O±CO₂ were added at the same time as the incompatible elements. An implication is that a significant proportion of the new continental crust generated since the Permian reflected multistage processes involving mobilization of continental mantle lithosphere that was enriched in minor and trace elements during the Proterozoic.     

Compositional diversity among Late Devonian peraluminous granitoid intrusions in the Meguma Zone of Nova Scotia, Canada

Late Devonian (385−370 Ma) granitoid intrusions in the Meguma Zone of southwestern Nova Scotia represent two geographically separate magmatic suites that show subtly different lithological, geochemical and isotopic characteristics. “Central intrusions” crop out with satellite mafic-intermediate intrusions, range in composition from granodiorite to leucogranite, contain two micas, have exclusively peraluminous compositions (molar A/CNK 1.1-1.3), variably high values for FeO_T (0.4–6.0 wt.%), Ba (5–980 ppm), Y (6–50 ppm), Pb (2–50 ppm), Ga (11–53 ppm), ⁸⁷Sr/⁸⁶Sr_i (0.7081-0.7130), δ¹⁸O (9.8–13.0) and δ³⁴S (4.5–11.9), in conjunction with low values for εNd (−1 to −6.5). In contrast, “peripheral plutons” crop out with synplutonic mafic-intermediate intrusions, range in composition from tonalite to leucogranite, may contain minor hornblende, have dominantly peraluminous compositions (molar A/CNK 0.9-1.3), variably high concentrations of TiO₂ (0.1-1.1 wt.%), Al₂O₃ (12.0–19.7 wt.%), CaO (0.2–4.9 wt.%), Sr (7–720 ppm), Cr (3–111 ppm) and V (1–136 ppm), higher εNd values (−2.0 to 3.2), and lower values for ⁸⁷Sr/⁸⁶Sr_i (0.7040-0.7079), δ¹⁸⁸O (7.6–10.5) and δ³⁴S (0–4.6). Such regional diversity is explained by inferring that upper crustal contamination dominated the central granitoid compositions and mixing with mantle-derived mafic-intermediate magmas dominated peripheral granitoid compositions. However, additional contributions from heterogeneous lower crust cannot be excluded.     

Occurrence and chemical composition of amphiboles and related minerals in corundum-bearing mafic rock from the Horoman Peridotite Complex, Japan

A corundum-bearing mafic rock in the Horoman Peridotite Complex, Japan, was derived from upper mantle conditions to lower crustal conditions with surrounding peridotites. The amphiboles found in the rock are classified into 3 types: (1) as interstitial and/or poikilitic grains (Green amphibole), (2) as a constituent mineral of symplectitic mineral aggregates with aluminous spinel at grain boundary between olivine and plagioclase (Symplectite amphibole) and (3) as film-shaped thin grains, usually less than 10 μm in width, at grain boundary between olivine and clinopyroxene (Film-shaped amphibole). The Film-shaped amphibole is rarely associated with orthopyroxene extremely low in Al₂O₃, Cr₂O₃ and CaO (Low-Al OPX). These minerals were formed by infiltration of SiO₂- and volatile-rich fluids along grain boundaries after the rock was recrystallized at olivine-plagioclase stability conditions, i.e. the late stage of the exhumation of the Horoman Complex.

Chondrite-normalized rare earth element patterns and primitive mantle-normalized trace-element patterns of the Green amphibole and clinopyroxene are characterized by LREE-depleted patterns with Eu positive and negative anomalies of Zr and Hf. These geochemical characteristics of the constituent minerals were inherited from original whole-rock compositions through a reaction involving both pre-existing clinopyroxene and plagioclase. We propose that the fluids were originally rich in a SiO₂ component but depleted in trace-elements. Dehydration of the surrounding metamorphic rocks in the Hidaka metamorphic belt, probably related to intrusion of hot peridotite body into the Hidaka crust, is a plausible origin for the fluids.     

鄂西南利川二叠纪吴家坪组硅质岩成因及沉积环境

鄂西南利川吴家坪组硅质岩与海相石煤及多层火山粘土岩共生,产海绵骨针及放射虫化石,放射虫组合以泡沫虫类为主,内射球虫类次之,隐管虫类很少,代表外陆棚沉积环境。硅质岩的陆源元素Al、Ti含量较高,热水来源元素Fe、Mn含量较低,Al/(Al+Fe+Mn)值在0.64~0.83之间,平均值0.73。在Al-Fe-Mn三角图中,样品位于或紧邻非热水沉积区,在 SiO₂- (K₂O+Na₂O)、SiO₂-Al₂O₃, (K₂O+Na₂O)-Al₂O₃ 图解中大多数样品落在火山成因区,少数位于火山成因与生物成因区之间。相对于沉积岩的微量元素丰度,生命元素Mo、V富集,指示热水沉积的特征元素Ba、As、Sc亏损。∑REE较低,∑LREE/∑HREE平均值为3.02,Ce、Eu均轻度负异常（δCe:0.75~0.83,平均值0.79;δEu:0.61~0.95, 平均值0.84）,经北美页岩标准化后稀土元素配分曲线近水平。以上地球化学特征表明研究区硅质岩属火山成因,并伴有生物作用。氧化还原判别指标U/Th、V/(V+Ni)及Ce_anom,沉积环境判别指标MnO/TiO₂,La_N/Yb_N 与判别图解100×TFe₂O₃/SiO₂-100 Al₂O₃/SiO₂、TFe₂O₃/(100-SiO₂)-Al₂O₃/(100-SiO₂)、TFe₂O₃/TiO₂-Al₂O₃/(Al₂O₃+TFe₂O₃)、La_N/Ce_N-Al₂O₃/(Al₂O₃+TFe₂O₃)与∑LREE/∑HREE-100×Eu/∑REE一致表明硅质岩形成于大陆边缘缺氧环境。     

渤海东部晚更新世以来的沉积物地球化学特征

为探讨渤海东部晚更新世以来的元素地球化学特征及控制因素,对渤海东部DLC70-1孔157个沉积物样品进行了化学成分、粒度及测年分析。结果表明,晚更新世以来研究区沉积物的物质来源与沉积环境较为稳定;根据DLC70-1孔沉积物地球化学特征,钻孔岩芯可划分为6层,反映了末次间冰期（暖期）晚期以来渤海东部沉积物物源的变化以及海面波动。Al₂O₃、MgO、TFe₂O₃、MnO、TiO₂、Cu、Zn、Pb、Cr和Rb等元素与细粒沉积物呈正相关,SiO₂、Na₂O与粗粒沉积物呈正相关,K₂O、Sr和Ba分布与沉积物粒度无明显正或负的相关性;R-型因子分析得出三种主要组合类型,以Mg、Sr和Ba为代表,分别对应陆源细粒物质输入与黄河物质、海河物质和滦河物质的影响。运用Ba/Al₂O₃与Sr/Al₂O₃、MgO/Al₂O₃与K₂O/Al₂O₃离散图分析了DLC70-1孔的物质来源,结果表明沉积物主要来源于黄河,该孔中上部32.30~49.00 m和9.30~23.20 m沉积物受到了滦河和海河物质的影响。     

Rapid analysis with energy-dispersive X-ray fluorescence spectrometry for bauxite investigation on the Mambilla Plateau, North Eastern Nigeria

Bauxite exploration involves routine analysis of a large number of samples for a wide range of elements. In Nigeria, though geological field exploration for bauxite started almost three decades ago very little has been achieved, mainly due to the non-availability of facilities for evaluating the dozens of suspected bauxite deposits scattered around the country. In this regard, a procedure for the rapid, accurate and precise measurement of a number of important elements in bauxite has been developed based on the newly acquired radioisotope based EDXRF spectrometer. Elements and oxides analyzed are Al₂O₃, SiO₂, TiO₂, Fe₂O₃, K₂O, Mn, Co, Cu, Zn, Ga, Rb, Sr, Y, Zr, Nb and Pb. The richest bauxite sample has concentrations of 48.08, 18.90, 1.26, 7.71 and 1.93 wt% for Al₂O₃, SiO₂, TiO₂, Fe₂O₃, and K₂O, respectively. The other values in ppm are Mn (3 0 2), Co (5 3 2), Cu (45), Zn (51), Ga (41), Rb (32), Sr (2 2 2), Y (32), Zr (8 4 9), Nb (89) and Pb (72). The measurement errors in terms of accuracy and precision are less than 5% and 10% and 5% and 15% for major and trace elements, respectively. Statistical correlation analysis carried out on the results shows the most significant relationships to be the negative correlations of alumina with silica, iron oxide and titanium. This is believed to be related to the processes of formation of bauxite, with the Si and Fe–Ti being removed as Al was being enriched.     

斯里兰卡普塔拉姆地区ZK593号钻孔沉积物的地球化学特征及意义

根据岩性、主微量元素特征和元素比值分析,斯里兰卡普塔拉姆地区ZK593钻孔的沉积物可分为6段。它们分别沉积于温暖潮湿、水动力较强的浅海-滨海相环境,经历了3次明显的海水进退。各层北美页岩标准化曲线平缓,轻重稀土元素没有明显的分异,Ce轻度亏损,球粒陨石标准化曲线斜率为负,轻稀土元素相对富集,各层Eu亏损明显,Ce轻度亏损,表明沉积物属于受陆源影响的陆棚沉积物。Ce负异常与碳酸盐沉积及气候环境有关。元素相关系数分析表明,Ca和Sr与生物作用关系明显;ΣREE与Al₂O₃和SiO₂等微量元素与陆源碎屑关系密切。δ¹⁸ O 的负向偏移与沉积后地下水的作用有关。