基于Apollo15月壤和普通球粒与碳质球粒陨石模拟实验的太空风化特征产物成因分析

月球、小行星等无大气行星体具有独特的反射光谱太空风化改造特征,其成因主要被归结于纳米级—亚微米级不透明颗粒等太空风化特征产物。本研究结合Apollo返回月壤样品、普通球粒和碳质球粒陨石样品的模拟实验结果,综合分析了太空风化特征产物的来源和成因,并讨论了其可能的光谱效应。研究结果表明,np-Fe⁰(纳米级单质金属铁)是铁镁硅酸盐等矿物经过微陨石轰击引起的气化沉积作用和原位还原作用形成。np-FeNi(纳米级铁镍金属)的成因主要包括FeNi金属和陨硫铁的气化沉积与冲击分散成因。np-FeNiS(纳米级铁镍金属的硫化物)和sm-FeNiS(亚微米级铁镍金属的硫化物)主要形成于陨硫铁的冲击分散过程。上述不透明颗粒是形成月球与S型小行星紫外—近红外波段光谱反射率降低、特征吸收峰减弱和连续统红移等特征的主要原因。气泡结构主要形成于层状硅酸盐等矿物在微陨石轰击过程中的挥发分逃逸,推测是含水量较高的小行星(如Bennu)紫外-近红外波段光谱反射率增加和连续统蓝移等特征的主要成因。实验结果预期对月球与小行星返回样品分析以及反射光谱的太空风化改造特征的解释提供一定的参考。     

顾及太空风化效应的虹湾地区矿物含量反演

月表矿物含量反演是研究月球地质起源和演化的关键.太空风化作用普遍发生在月球表面,对矿物纯净光谱造成了不可忽视的影响,它弱化光谱吸收特征, 降低反射率,影响矿物含量遥感反演精度.基于Relab光谱库和Hapke辐射传输模型,将月表 4种矿物(单斜辉石、斜方辉石、斜长石、橄榄石)的二向性反射率转换成同向性的单次散射反照率,然后计算矿物的光学常数;再根据亚微观金属铁SMFe(submicroscopic metallic iron)的质量分数模拟6种不同程度太空风化效应,得到端元矿物的反射率光谱;最后基于上述方法,利用多端元线性分解方法和M3(moon mineralogy mapper,月球矿物绘图仪)高光谱数据反演不同风化程度下的矿物含量,得到月表虹湾地区辉石、斜长石、橄榄石3种矿物的含量分布.实验表明,利用多端元线性分解可以有效模拟太空风化效应对矿物光谱的影响,是研究太空风化效应影响下矿物识别及含量反演的一种行之有效的方法.      

Experimental Model of the Formation of Nanophase Metallic Iron in the Lunar Regolith

Doklady Earth Sciences - One of the signs of “space weathering” on the Moon, including the effect of the solar wind and micrometeorite bombardment, is the formation of nanophase...     

月壤颗粒微观环带的太空风化成因

太空风化是迄今31亿年以来影响月球表面物质演化过程的主要因素,主要包括陨石、微陨石的轰击,太阳风粒子的注入,太阳/银河宇宙射线的辐射以及周期性的加热作用等。通过深入剖析太阳风粒子的注入与溅射、微陨石轰击的蒸发与沉积、宇宙射线辐射的辐射损伤等过程的作用机理,探讨了不同太空风化过程对矿物颗粒环带厚度、化学组成、晶体结构等特征的影响,认为微陨石轰击与太阳风注入是形成月壤颗粒微观环带的主导因素,宇宙射线辐射与周期性加热的影响可忽略不计。进一步结合非晶质环带、富内含物环带、多环环带以及小泡环带等月壤颗粒主要环带的基本特征,在总结和对比分析各类型环带的厚度、结构以及化学组成特征基础上,对不同类型环带的成因进行初步推断,认为非晶质环带、小泡环带以及多环环带的内层环带具有太阳风作用特征,而富内含物环带、多环环带的外层环带则具有微陨石轰击的成因特征。根据目前单纯依靠环带的化学组成分析解释环带成因存在的不足,指出了通过补充分析矿物晶体结构在模拟太空风化实验过程中的变化特征来研究环带成因的新思路。     

Spectroscopic evidence for aqueous alteration products on the surfaces of low-albedo asteroids

High-resolution IR spectra (0.9–2.5 μm) and narrowband photometry (3.0–3.5 μm) are presented for asteroids 1 Ceres, 2 Pallas and 324 Bamberga. Laboratory experiments with hydrated minerals indicate that the 3 μm absorption feature observed on asteroids is largely due to interlayer water molecules in clay minerals, with a possible contribution from water molecules bound to salts. The depth of the 3 μm band as a function of 2.2 μm albedo is a useful measure of the amount of hydrated mineral present on these asteroids. 1 Ceres must consist mostly of a clay mineral like that in CM chondrites, with some contribution to the strength of the 3 μm band by hydrated salts. These salts, which are products of aqueous alteration, may also be responsible for Ceres' high albedo relative to other C-type asteroids. 2 Pallas must have a low abundance of hydrated minerals relative to 1 Ceres, with the bulk of its composition being spectrally featureless minerals such as the iron-free silicates in CM chondrules. 324 Bamberga probably contains clay minerals, but their abundance cannot be determined at present. The spectrum of Bamberga below 2.5 μm shows evidence for abundant magnetite, which can be a product of aqueous alteration. The presence of magnetite on Bamberga and possibly other C-type asteroids may be responsible for their low albedos. The spectra of C-type asteroids may be reconcilable with those of carbonaceous chondrites if the asteroids surfaces have undergone alteration by aqueous or other analogous processes.     

Selective detection of Fe and Mn species at mineral surfaces in weathered granite by conversion electron yield X-ray absorption fine structure

A new method for the speciation of Fe and Mn at mineral surfaces is proposed using X-ray absorption fine structure in conversion electron yield mode (CEY-XAFS). This method generally reflects information on the species at the sub-μm scale from the particle surface due to the limited escape depth of the inelastic Auger electron. The surface sensitivity of this method was assessed by experiments on two samples of granite showing different degrees of weathering. The XANES spectra of the Fe-K and Mn-K edge clearly gave different information for CEY and fluorescence (FL) modes. These XANES spectra of Fe and Mn show a good fit upon application of least-squares fitting using ferrihydrite/MnO₂ and biotite as the end members. The XANES spectra collected by CEY mode provided more selective information on the secondary phases which are probably present at the mineral surfaces. In particular, CEY-XANES spectra of Mn indicated the presence of Mn oxide in unweathered granite despite a very small contribution of Mn oxide being indicated by FL-XANES and selective chemical-extraction analyses. Manganese oxide could not be detected by micro-beam XANES (beam size: 5 × 5 μm²) in unweathered granite, suggesting that Mn oxide thinly and ubiquitously coats mineral surface at a sub-μm scale. This information is important, since Mn oxide can be the host for various trace elements. CEY-XAFS can prove to be a powerful tool as a highly sensitive surface speciation method. Combination of CEY and FL-XAFS will help identify minor phases that form at mineral surfaces, but identification of Fe and Mn oxides at mineral surfaces is critical to understand the migration of trace elements in water-rock interaction.     

Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces

The reststrahlen features in thermal infrared, or vibrational, spectra of Mg-Fe olivines ((Mg,Fe)₂SiO₄) exhibit trends in position, strength, and number of features that are diagnostic of the relative proportions of the Mg and Fe cations in the minerals. Although band positions move to lower wavenumbers (longer wavelengths) across the forsterite–fayalite compositional binary in a generally linear manner, specific feature shifts in transmittance data are described best by two linear fits with a break in slope near Fo₇₀. The break in slope may be accompanied by an offset as well; both traits are attributed to structural changes in olivine brought about by distortion of the crystal lattice by Fe. Reflectance and emissivity spectra exhibit similar trends in band position with composition, and all three types of data demonstrate that some olivine band strengths change across the Mg–Fe solid solution series and also are diagnostic of composition. Olivines have been identified in a wide array of thermal infrared spectra of planetary materials and have been interpreted as being present on the surfaces of Mercury, the Moon, Mars, and a number of asteroids based on the analysis of thermal infrared spectra. New linear least squares models of the emissivity spectra of olivine-bearing Martian meteorites enable a preliminary estimation of the accuracy with which quantitative estimates of olivine abundance and solid solution composition can be derived from the spectra of mixtures.     

辽宁兴城地区岩石光谱测试及特征分析

在辽宁兴城野外实习基地采用ASD光谱仪完成不同岩石样品光谱测试的基础上, 分析了不同类型、不同地质时代的岩浆岩和沉积岩, 及其风化面和新鲜面的光谱曲线特征。兴城野外不同岩浆岩与沉积岩光谱曲线形态相似, 新鲜面和风化面的特征光谱吸收位置相差不大, 但新鲜面的反射率普遍高于风化面的反射率;岩浆岩和沉积岩样品一般在波长为900 nm左右存在铁离子吸收谷;除了在1 400 nm和1 900 nm处有水汽吸收带外, 岩浆岩和沉积岩样品在2 200 nm左右还存在强吸收谷, 而灰岩在2 300 nm左右有比较高的吸收谷, 这也是利用实测光谱进行岩性分类的理论基础。但是, 不同地质年代下的岩石光谱曲线变化并无规律, 更多地与岩石结构、成分和环境因素等相关。这样, 岩石光谱测试及其特征分析可满足研究区岩性识别、矿化蚀变信息提取的需要。     

Mineralogy and spectroscopy (visible near infrared and Fourier Transform Infrared) of Mukundpura CM2: Implications for asteroidal aqueous alteration

We report the textures, mineralogy and mineral chemistry of the Mukundpura matrix component, a clast-bearing, brecciated, new CM2 carbonaceous chondrite. Like other CMs, Mukundpura is matrix-enriched and has experienced different degrees of aqueous alteration with evidences of fracturing and compaction of clasts due to the impact. A few relict chondrule clasts and CAIs (diopside and spinel) survived despite of the alteration amidst accessory phases of olivine, magnetite, sulphides and calcite. X-Ray Diffraction (XRD), Visible Near Infrared (VNIR) and Fourier Transform Infrared (FTIR) spectroscopic studies reveal higher phyllosilicate content (∼90 %) comprising of both Mg and Fe-serpentine and abundant serpentine-sulphide intergrowths. Even then, the presence of accessory olivine as relict clasts can be interpreted from the presence of certain typical olivine absorptions in the FTIR spectra. The non-stoichiometric, Tochilinite-Cronstedtite occurrences probably relate to broadening of XRD and FTIR spectra and can be explained by coupled Al–Si and Mg–Al substitutions in talc and serpentine. The FTIR spectra suggest widespread transformation of olivine to serpentine, unlike the largely unaltered chondrules. The correlations of mineralogical alteration index with FeO/SiO₂ and S/SiO₂ in different domains of matrix suggest different extent of alterations. Thus, the aqueous alteration is extensive but not pervasive. The majority of alteration seems to have occurred within the asteroidal parent body. The Mukundpura CM2 thus preserves a unique combination of relict chondrules and highly aqueous altered variegated matrix clasts, although the surface mineralogy resembles the C-type asteroids recently probed by OSIRIS-REx and Hayabusa-2 missions.     

玄武岩微生物分解过程中的矿物表面效应

通过玄武岩微生物风化的模拟实验,探讨了造岩矿物表面特征对微生物风化的影响,发现在细菌Paeni-bacillus polymyoca(多粘芽孢杆菌)及其代谢产物的作用下,玄武岩的分解作用显著增强,其中橄榄石最易分解,辉石次之,长石则相对最稳定.根据实验溶液的成分变化,认为橄榄石在初始阶段的分解主要受控于表面化学特征,随着比表面积的增大,表面控制作用进一步增强,分解更为快速.     

烟曲霉对蛇纹石和橄榄石的风化作用

含镁硅酸盐矿物是重要自然资源,国内外大都采用传统的化学方法进行开发利用,而微生物法释放含镁硅酸盐矿物中镁和硅的研究还未见报道.试验采用摇瓶培养与对照结合的方法研究烟曲霉(Aspergillusfumigatus)对含镁硅酸盐矿物——蛇纹石和橄榄石的风化作用.试验采用ICP-OES测定第5、10、20、30 d培养液滤液...     

FTIR spectroscopy of OH in olivine: A new tool in kimberlite exploration

Our study of olivines from Canadian kimberlites shows that the application of FTIR spectroscopy significantly improves the reliability of olivine as a kimberlite indicator mineral (KIM). We have developed an algorithm that yields the water concentration and the normalized intensity of the OH IR absorption band at 3572 cm⁻¹ from unpolished olivine grains of unknown thickness. For 80% of kimberlitic olivines these two parameters are significantly higher than those for olivines from non-kimberlitic magmas and consequently, olivines with water concentrations >60 ppm and a strong absorption band at 3572 cm⁻¹ can be reliably classified as being kimberlitic.We have identified two major spectral features in the OH absorption bands of kimberlitic olivines that allow for a more detailed classification: (a) the presence of three types of high-requency OH absorption bands (Group 1A, 1B and 1C) and (b) the proportion of low-frequency OH absorption bands (Group 2) relative to high-frequency bands (Group 1). Comparison of our results with experimental studies suggests that differences within Group 1 OH absorption bands are due to different pressures of crystallization or hydrogenation. The three identified types of Group 1 OH absorption bands approximately correspond to high (P > 2 GPa, Group 1A), moderate (2-1 GPa, Group 1B), and low (<1 GPa, Group 1C) pressures of hydrogenation. Group 2 OH IR absorption bands in olivines with NiO > 3500 ppm are interpreted to reflect olivine-orthopyroxene equilibria and hence are indicative of xenocrystic olivine derived from lherzolitic or harzburgitic mantle sources. Interaction of xenocrystic olivine with hydrous kimberlitic melts with low silica activity likely will cause a gradual increase in Group 1 absorption bands. Therefore, FTIR spectra of olivine can be used to obtain qualitative estimates of the duration of interaction between mantle material and a kimberlitic melt.In addition to applications in kimberlite and diamond exploration, FTIR spectra of olivine phenocrysts, combined with mineral chemical data, may also provide insights into kimberlite evolution. Our data suggest that in some instances the ascent of kimberlitic magmas could have been interrupted at or near the Moho, followed by olivine crystallization and exsolution of aqueous fluids.     

The stability of ortho- and clinopyroxenes,olivine, and garnet in kimberlitic magma

It is generally accepted that the composition of ultrabasic nodules and their quantitative proportions do not significantly change during their transportation with kimberlitic magma to the Earth’s surface. We performed an experimental study of the relative stability of olivine, garnet, and pyroxenes in kimberlite melt at high pressure and temperatures (4 GPa, 1300–1500 °C). The study has shown that the loss in weight of minerals and, correspondingly, the rate of their dissolution in kimberlite melt differ considerably. The following sequence of the dissolution rates of minerals has been established: Cpx ≥ Opx > Gar > Ol. Pyroxenes are characterized by the most rapid dissolution, and olivine is the most stable mineral. The assumption is made that clinopyroxenites and websterites disintegrate more rapidly than dunites and lherzolites in kimberlitic magma.     

The dissolution of olivine added to soil: Implications for enhanced weathering

Chemical weathering of silicate minerals consumes atmospheric CO₂ and is a fundamental component of geochemical cycles and of the climate system on long timescales. Artificial acceleration of such weathering (“enhanced weathering”) has recently been proposed as a method of mitigating anthropogenic climate change, by adding fine-grained silicate materials to continental surfaces. The efficacy of such intervention in the carbon cycle strongly depends on the mineral dissolution rates that occur, but these rates remain uncertain. Dissolution rates determined from catchment scale investigations are generally several orders of magnitude slower than those predicted from kinetic information derived from laboratory studies. Here we present results from laboratory flow-through dissolution experiments which seek to bridge this observational discrepancy by using columns of soil returned to the laboratory from a field site. We constrain the dissolution rate of olivine added to the top of one of these columns, while maintaining much of the complexity inherent in the soil environment. Continual addition of water to the top of the soil columns, and analysis of elemental composition of waters exiting at the base was conducted for a period of five months, and the solid and leachable composition of the soils was also assessed before and after the experiments. Chemical results indicate clear release of Mg²⁺ from the dissolution of olivine and, by comparison with a control case, allow the rate of olivine dissolution to be estimated between 10^−16.4 and 10^−15.5 moles(Mg) cm⁻² s⁻¹. Measurements also allow secondary mineral formation in the soil to be assessed, and suggest that no significant secondary uptake of Mg²⁺ has occurred. The olivine dissolution rates are intermediate between those of pure laboratory and field studies and provide a useful constraint on weathering processes in natural environments, such as during soil profile deepening or the addition of mineral dust or volcanic ash to soils surfaces. The dissolution rates also provide critical information for the assessment of enhanced weathering including the expected surface-area and energy requirements.     

An experimental model approach of biologically-assisted silicate dissolution with olivine and Escherichia coli – Impact on chemical weathering of mafic rocks and atmospheric CO2 drawdown

Chemical weathering of Mg, Ca-silicates and alumino-silicates contributes significantly to the drawdown of atmospheric CO₂ over long time scales. The present work focuses on how this mode of weathering may change in the presence of free-living bacteria in oligotrophic waters, which compose most of the surface freshwaters of the Earth. Forsterite (Fo90) was reacted for 1 week with a stable Escherichia coli population in water maintained at 37 °C and neutral pH in a batch reactor. Control samples with suspensions of pure olivine powders and E. coli cells in pure water were also used for reference. Olivine controls reproduce the Mg, Si and Fe release in solutions predicted from rates published in the literature with pH shifts of less than 0.5 unit. After 1 week, under abiotic conditions, weathered surfaces are enriched in Fe and Fe³⁺ relative to the initial composition of the mineral. Bacterial controls (without minerals) show decreasing Eh with increasing cell concentrations (−50 mV with 7 × 10⁷ cells/mL and −160 mV with 8 × 10⁸ cells/mL). Magnesium concentrations in bacterial control solutions are in the μg/L range and can be accounted for by the release of Mg from dead cells. More than 80% of the cells were still alive after 1 week. The solutions obtained in the experiments in which olivine reacts in the presence of cells show Mg and Si concentrations a few tens of percent lower than in the mineral control samples, with a prominent depletion of Fe(III) content of the mineral surfaces. Magnesium mass balance discounts both significant bacterial uptake and inhibition of the Mg dissolution rates as a consequence of changing pH and Eh. Coating by bacterial cell layers is also negligible. E. coli reduces the chemical weathering of olivine. This study infers that the presence of free-living Proteobacteria, a prevalent group of subsurface bacteria, should decrease the amount of riverine Mg released by chemical weathering of mafic rocks.     

不同粒径的月球橄榄石二向性反射特征研究

研究月表矿物组成和分布,对于探测月表地质构造以及月球的起源和演化具有重要的意义。因此,物质成分探测一直是月球研究的重点课题之一。尽管人类已经能够从月球采集样品进行实验室分析,但遥感技术仍然是研究月球的主要手段。文中主要目的是模拟不同粒径下橄榄石的二向性反射特征。为此,首先提出模拟不同粒径下反射特征的方法,然后利用Hapke模型和Mie散射理论对不同粒径下富铁和富镁橄榄石的二向性反射特征进行了模拟。模拟结果显示,富镁橄榄石的二向性反射率较富铁橄榄石的反射率高。最后,分析了反射率差值和等效粒径的相关性。该结论为选择探月传感器的波段组合、识别橄榄石镁铁含量提供了理论依据,也为应用遥感数据的橄榄石的判别奠定了基础。     

Oxygen isotope measurements of individual unmelted Antarctic micrometeorites

We present oxygen isotope measurements of 28 unmelted Antarctic micrometeorites measuring 150-250 μm (long axis) collected in the South Pole water well. The micrometeorites were all unmelted and classified as either fine-grained, scoriaceous, coarse-grained or composite (a mix of two other classes). Spot analyses were made of each micrometeorite type using an ion microprobe. The oxygen isotope values were measured relative to standard mean ocean water (SMOW) and range from δ¹⁸O = 3‰ to 60‰ and δ¹⁷O = −1‰ to 32‰, falling along the terrestrial fractionation line (TFL) within 2σ errors. Several analytical spots (comprising multiple phases) were made on each particle. Variability in the oxygen isotope ratios was observed among micrometeorite types, between micrometeorites of the same type and between analytical spots on a single micrometeorite indicating that micrometeorites are isotopically heterogeneous. In general, the lowest isotope values are associated with the coarse-grained micrometeorites whereas most of the fine-grained and scoriaceous micrometeorites have an average δ¹⁸O ? 22‰, suggesting that the matrix in micrometeorites is isotopically heavier than the anhydrous silicate phases. The oxygen isotope values for the coarse-grained micrometeorites, composed mainly of anhydrous phases, do not lie along the carbonaceous chondrite anhydrous mineral (CCAM) line, as observed for olivines, pyroxenes and some kinds of chondrules in carbonaceous chondrites, suggesting that coarse-grained MMs are not related to chondrules, as previously thought. Our measurements span the same range as values found for melted micrometeorites in other studies. Although four of the micrometeorites have oxygen isotope values lying along the TFL, close to the region where the bulk CI carbonaceous chondrites are found, 21 particles have very enriched ¹⁷O and ¹⁸O values that have not been reported in previous analyses of chondrite matrix material, suggesting that they could be a new type of Solar System object. The parent bodies of the micrometeorites with higher ¹⁸O values may be thermal metamorphosed carbonaceous asteroids that have not been found as meteorites either because they are friable asteroids that produce small particles rather than rocks upon collision with other bodies, or because the rocks they produce are too friable to survive atmospheric entry.     

Correlation analysis and partial least square modeling to quantify typical minerals with Chang＇E-3 visible and near-infrared imaging spectrometer＇s ground validation data

In 2013, Chang＇E-3 program will develop lunar mineral resources in-situ detection. A Visible and Near-infrared Imaging Spectrometer （VNIS） has been selected as one payload of CE-3 lunar rover to achieve this goal. It is critical and urgent to evaluate VNIS＇ spectrum data quality and validate quantification methods for mineral composition before its launch. Ground validation experiment of VNIS was carried out to complete the two goals, by simulating CE-3 lunar rover＇s detection environment on lunar surface in the laboratory. Based on the hyperspectral reflectance data derived, Correlation Analysis and Partial Least Square （CA-PLS） algorithm is applied to predict abundance of four lunar typical minerals （pyroxene, plagioclase, ilmenite and olivine） in their mixture. We firstly selected a set of VNIS＇ spectral parameters which highly correlated with minerals＇ abundance by correlation analysis （CA）, and then stepwise regression method was used to find out spectral parameters which make the largest contri- butions to the mineral contents. At last, functions were derived to link minerals＇ abundance and spectral parameters by partial least square （PLS） algorithm. Not considering the effect of maturity, agglutinate and Fe~, we found that there are wonderful correlations between these four minerals and VNIS＇ spectral parameters, e.g. the abundance of pyroxene correlates positively with the mixture＇s absorption depth, the value of absorption depth added as the in- creasing of pyroxene＇s abundance. But the abundance of plagioclase correlates negatively with the spectral parame- ters of band ratio, the value of band ratio would decrease when the abundance of plagioclase increased. Similar to plagioclase, the abundance of ilmenite and olivine has a negative correlation with the mixture＇s reflectance data, if the abundance of ilmenite or olivine increase, the reflectance values of the mixture will decrease. Through model validation, better estimates of pyroxene, plagioclase and ilmenite＇s abundances are given. It is concluded that VNIS has the capability to be applied on lunar minerals＇ identification, and CA-PLS algorithm has the potential to be used on lunar surface＇s in-situ detection for minerals＇ abundance prediction.     

Reflectance spectrophotometry extended to u.v. for terrestrial,lunar and meteoritic samples

Extension of remote sensing of planetary bodies to the ultraviolet is now feasiable up to 2000 Å from earth-orbiting telescopes and spacecraft. The benefits of this extension is analysed on the basis of laboratory spectra taken on a large variety of terrestrial, lunar and meteoritic samples. Knowledge of the albedo for two wavelengths at 2300 and 6500 Å permits classification of a surface into one of the following types: lunar, carbonaceous chondrites, ordinary chondrites, achondrites or acidic rocks, basaltic rocks, irons. For lunar-type surfaces, a simple albedo measurement at 6500 Å can be converted into quantitative abundance determinations of silicate, aluminium oxide and iron; a large amount of telescopic lunar photometry data is available for mapping these abundances. Extension of the photometry to 2300 Å permits quantitative measurement of TiO₂ abundances. For asteroids and non-icy satellites, rock-type classification and constraints in chemical abundances of Si, Al, Fe and Ti can be derived from photometry at 2300 and 6500 Å. The IUE telescope already orbiting the earth, the Space Telescope to come, the lunar polar orbiter and other spacecraft under prospect are potentially available to provide the photometric observations at 6500 and 2300 Å required.     

Quantitative Untersuchungen mit der Elektronen-Mikrosonde an Pyroxenen aus Basalten und Peridotit-Einschlüssen

The chemical composition of the pyroxenes and olivines of 12 basaltic rocks and 5 lherzolite nodules was determined quantitatively by electron micro-probe analysis. The composition of the pyroxenes depends on the type of basalt in which they occur. Tholeiitic basalts with normative quartz contain three pyroxenes: orthorombic pyroxenes, pigeonites and augites. All pyroxene phases are zoned and do not show any exsolution. Their Ti and Al contents (Ca-Tschermaks and Ti-augite molecules) are small. All pyroxene phases were formed under disequilibrium with each other and with the melt because of rapid quenching. The sequence of crystallization: orthopyroxene—pigeonite—augite could be established by their Cr content.The alkali olivine basalts undersatured in SiO₂ and the olivine nephelinites are characterized by Ti and Al-rich clinopyroxenes. The distribution of Ti and Al in the pyroxenes of the alkali olivine basalts shows a differentiation trend from the cores of the phenocrysts to their outer zones and to the crystals of the ground mass. Thereby the Ca-Tschermaks molecule is being replaced more and more by the Ti-augite molecule. The Ti content of the pyroxenes of the olivine nephelinites decreases in the last stage of differentiation because simultaneously increasing amounts of titaniferous magnetite crystallize.The pyroxenes of lherzolite peridotite nodules are characterized by high Al and low Ti contents which differ according to the type of basalt (alkali olivine basalt or olivine nephelinite) in which the nodules occur. The homogeneous distribution of the elements within the single grains indicates crystallization under equlibrium conditions. The conditions of their formation are comparable to those of Al-pyroxene peridotites in the upper mantle. The composition of pyroxenes of early accumulates of alkali basaltic melts differ from those of peridotite nodules. Therefore lherzolite nodules can be taken as residues of deeper peridotite masses.