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本文报道了辽宁弓长岭二矿区太古宙纹层状斜长角闪岩中微球粒之发现。微球粒一种呈暗色、不透明、有磁性;另一种为浅乳黄—棕黄色、透明—半透明、无磁性或弱磁性。它们多为玻璃质,强磁性者为磁铁矿。微球粒具气孔、瘤状、气泡塌陷、连体、凹坑等反映强塑性、高速运动、富挥发份、快速冷凝特征的多种表面和内部结构。其化学组成以SiO_2、TFe、Al_2O_3和CaO为主。它们的形成可能与火山作用或陨石撞击作用有关。无论其成因如何,均表明:1)纹层状斜长角闪岩的原岩为基性凝灰岩;2)本区变质温压条件存在微区不均匀性。 相似文献
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剑阁球粒陨石于1964年10月9日(或19日),陨落于四川省剑阁县杨家村公社民主大队。1964年12月,经四川省地质局实验室涂继尧等同志初步定为石陨石。1966年3月,我所钟大赉和刘秉光两同志,由四川省地质局实验室得到一小块大小为6.2×5×1.8公分,重222克的标本(照片1)。陨石的原形和大小现已无法查清。恩施球粒陨石于1974年12月26日15时30分陨落于湖北省恩施县芭蕉区,地理坐标东经109°51′20″,北纬30°34′40″。1977年9月,笔者赴现场调查时,据直接了解情况的李建华同志介绍,当时在瓦屋公社、乾溪公社和寨湾公社交界处的上空,突然由西北往东南方向发出声响,在70-80里的范围内都能听见。尔后掉下多块陨石。 相似文献
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湖南宁乡钾镁煌斑岩中火山微球粒的初步研究 总被引：3，自引：0，他引：3
本次研究从钾镁煌斑岩中挑选出上万个微球粒进行了系统研究。微球粒有三种：无磁性无色透明—半透明浅黄色、棕褐色至不透明黑色；弱磁性—强磁性黑色；强磁性钢灰色铁质。除微球粒外，还有岩浆溅射碎片和炉渣伏溅射碎片等火山尘。微球粒具有火山喷发条件下可出现的多种多样的表面结构和内部结构。其化学成分主要为：（１）贫铁型，富Ｓｉ、Ｍｇ、Ｃａ、Ｐ，贫Ｔｉ、Ｍｎ、Ｋ；（２）富铁型，富Ｓｉ、Ｔｉ、Ｍｎ、Ｋ，贫Ｃａ、Ｍｇ、Ｐ；（３）高铁型，以Ｆｅ为主。单个微球粒中还出现高Ｓｉ相和高Ｓｉ、Ｍｇ相。据微球粒化学成分的多样性推测，在钾镁煌斑岩浆侵位至地壳深部环境下，经历过液态熔离作用，当火山喷发时，在快速冷凝条件下形成火山微球粒。 相似文献
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四川重庆中梁山P/T界线粘土层中非粘土组分的研究 总被引：9，自引：0，他引：9
本文报道了四川重庆中梁山P/T界线粘土层中的非粘土组分及其研究成果,包括具似文象结构的铁质微球粒,硅质、石质微球粒以及各种碎屑矿物。认为除了具似文象结构的铁质微球粒可能属地外成因外,其他微球粒和碎属矿物均为火山作用产物。 相似文献
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首次报道齐依求金矿中微球粒的发现，对微球粒形态特征、表面及断面结构、物理特性、矿物组成、化学成分进行分析测试，并就其成因作了初步探讨，认为属宇宙成因。 相似文献
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宁强碳质球粒陨石的球粒和基质中出现大量圆形的不透明矿物集合体。其中的主要矿物为磁铁矿、富镍金属和硫化物，另有少量磷酸盐、硅酸盐及微量的铂族金属。离子探针测定显示：①磁铁矿的氧同位素组成服从质量分馏[斜率为0.51±0.04,Δ17O为（-2.8±0.4)‰],δ18O值在-15.3‰~-1.6‰的较大范围内变化；②球粒中的橄榄石(Δ17O为-5.0‰）与不透明矿物集合体处于氧同位素不平衡状态。不透明矿物集合体是由小行星母体中的蚀变反应产生的，金属铁被氧化为磁铁矿，同时使剩余的金属富集镍。 相似文献
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本文对南丹IIICD铁陨石的矿物学特征进行了研究,并与同为铁陨石但化学分类不同的阿根廷IAB铁陨石和西伯利亚IIB铁陨石进行了对比,重点探讨了风化作用对铁陨石矿物学特征的影响.首先用偏光显微镜、静水称重、扫描电镜观察了样品的基本矿物学特征和微形貌特征,然后用振动式样品磁强计、X射线衍射与电子探针能谱半定量测试研究了样品的磁学性质、物相和化学组成.研究结果表明,南丹铁陨石在较强的自然风化作用下,光泽变弱为土状光泽,相对密度降低;风化产生的反铁磁性物质会使陨石的磁性下降;另外,样品表面物相组成也发生较大变化,以针铁矿(FeOOH)和磁铁矿(Fe3O4)等铁的次生矿物为主;但风化壳以下的矿物物相及化学成分均未发生明显变化,以Fe、Ni为主的铁纹石、镍纹石物相存在. 相似文献
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Petrographic, mineralogical and chemical analysis of naturally weathered equilibrated ordinary chondrites collected from ‘ hot’ deserts and Antarctica has revealed striking similarities and also pronounced differences in weathering between the two environments. Terrestrial weathering in all meteorites studied is dominated by oxidation and hydration of Fe,Ni metal, producing Fe-oxides and oxyhydroxides that have partially replaced the metal grains and have also occluded primary intergranular pores to form veins. Troilite weathers readily in ‘ hot’ desert environments but undergoes very little alteration under Antarctic conditions. Most of the primary porosity of ordinary chondrites has been occluded by the time that ∼ 15 to 25% of the initial Fe0 and Fe2+ has been oxidised to Fe3+ in both environments. Results from modelling the volume changes upon alteration of primary minerals to a range of weathering products demonstrates that the primary porosity of most meteorites is sufficient to accommodate weathering products. Dilation of primary pores and brecciation, which has been observed in parts of some meteorites, will only occur if the meteorite is especially metal-rich, or has a low primary porosity. These weathering products are absent from recent falls but have formed in a fall after ∼ 100 yr of museum storage.Cl-bearing akaganéite and hibbingite are common weathering products in Antarctic finds but occur in abundance in only one ‘ hot’ desert meteorite, Daraj 014. The majority of Fe-rich weathering products in meteorites from both environments contain low, but variable concentrations of Si, Mg and Ca. In most meteorites a proportion of these elements are inferred to be present as a very finely crystalline mineral with a ∼ 1.0-nm lattice fringe spacing; where seen within intragranular fractures this mineral has a topotactic relationship with olivine and orthopyroxene. In the heavily-weathered Antarctic finds ALHA 78045 and 77002, Si is concentrated in cronstedtite, a Fe-rich phyllosilicate. An unidentified hydrous Si-Fe-Ni-Mg mineral or gel has also partially replaced taenite in ALHA 78045. In addition to Fe-rich weathering products, ‘ hot’ desert meteorites contain sulphates, Ca-carbonate and silica, whereas such minerals are largely absent from Antarctic finds. The abundance of silicate weathering products in Antarctic meteorites is unexpected and indicates that olivine and pyroxene undergo significant chemical weathering in these environments. As preterrestrial cronstedtite is abundant in CM2 carbonaceous chondrites, the Antarctic environment may be a powerful analog for aqueous alteration in the asteroidal parent bodies of primitive meteorites. 相似文献
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Practically all of the examined spherules extracted in 1948?C1949 from soil at the crater field of the 1947 Sikhote Alin meteorite shower are ablation spherules produced during this meteorite fall. The spherules can classified into two textural types: (i) fine-grained, which consist of Ni-bearing magnetite (3?C6 wt % NiO) dendrites, sometimes with minor amounts of interstitial P- and Fe-rich material, and (ii) coarse-grained, which also consist of Ni-bearing magnetite dendrites or grains, sometimes with wuestite, an interstitial material, which resembles that in type (i) or has a silicate composition. The texture, mineralogy, and chemistry (presence of P and Si) of these spherules differ from those of iron cosmic spherules (type I) that occur in the background flux of micrometeorites. The spherules are thought to were produced by the ablation of meteoritic material at elevations of about 12 km (in the region where disintegration starts) and below, at maximum temperatures of 1600?C2180°C and oxygen fugacity of 10?14 to 10?1 atm. Conceivably, the ablated material was enriched in silicates compared to the fallen material. 相似文献
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Soil layers at the Tunguska event site may have accumulated infalling extraterrestrial matter derived from the Tunguska Cosmic
Body (TCB). Using mineralogical, textural, and chemical criteria, a set of metal and silicate spherules of probably cosmic
origin was identified in the collection of spherules and rounded particles recovered from sites with high concentrations of
magnetic spherules on a terrace above the floodplain of the Chunya River. The metal spherules consist of Ni(Cr)-bearing wüstite
and magnetite with Ni-rich metal inclusions. The silicate spherules are glassy, cryptocrystalline, barred, and porphyritic
melted micrometeorites, some of which contain metal droplets. The number of spherules counted in our samples is higher than
the background level, indicating the possible presence of the TCB material. 相似文献
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For most iron meteorites studied, the carbon isotopic composition of nodular graphite falls in the range ?4.8 to ?8.2%. vs PDB and shows a mode between ?5 and ?6%.. Fourteen cohenite analyses from the Magura meteorite fall between ?18.1 and ?19.2%. with a pronounced clustering around ?18.5%.. Carbon of a taenite separate from the same meteorite has an isotopic composition of ?18.8%.; compositions between ?19.7 and ?22.1%. were found for taenite carbon in five other octahedrites. It is suggested that the 12C enrichment in cohenite and taenite relative to the nodular graphite is a general phenomenon in iron meteorites, and that the study of 13C abundances in iron meteorites may aid in the elucidation of their history. To this end an experimental study of carbon isotope fractionations in the system Fe-Ni-C is essential. The 13C content of carbon from several silicate inclusions in the Four Corners and ‘El Taco’ (Campo del Cielo) meteorites is generally similar to the nodular graphite, the 12C enrichment (?13%.) in one specimen may be interpreted in terms of a mixing model involving an original inclusion carbon and carbon exsolved from the taenite upon cooling. 相似文献
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The paper reports scanning electron microscopy (FEG-SEM) and transmission electron microscopy (TEM) data on three cryptocrystalline (CC) cosmic spherules of chondritic composition (Mg/Si ≈ 1) from two collections taken up at glaciers at the Novaya Zemlya and in the area of the Tunguska event. The spherules show “brickwork” microtextures formed by minute parallel olivine crystals set in glass of pyroxene–plagioclase composition. The bulk-rock silicate chemistry, microtexture, mineralogy, and the chemical composition of the olivine and the local chemistry of the glass in these spherules testify to a chondritic source of the spherules. The solidification of the spherules in the Earth’s atmosphere was proved to be a highly unequilibrated process. A metastable state of the material follows, for example, from the occurrence of numerous nanometer-sized SiO2 globules in the interstitial glass. These globules were formed by liquid immiscibility in the pyroxene–SiO2 system. Troilite FeS and schreibersite (Fe,Ni)3P globules were found in the FeNi metal in one of the spherules, which suggests that the precursor was not chemically modified when melted in the Earth’s atmosphere. Our results allowed us to estimate the mineralogy of the precursor material and correlate the CC spherules with the chondrule material of chondrites. The bulk compositions of the spherules are closely similar to those of type-IIA chondrules. 相似文献
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Exsolutions of Diopside and Magnetite in Olivine from Mantle Dunite, Luobusa Ophiolite, Tibet, China 总被引：1，自引：0，他引：1
The exsolutious of diopside and magnetite occur as intergrowth and orient within olivine from the mantle dunite, Luobusa ophiolite, Tibet. The dunite is very fresh with a mineral assemblage of olivine （〉95%） ＋ chromite （1%-4%） ＋ diopside （〈1%）. Two types of olivine are found in thin sections： one （Fo = 94） is coarse-grained, elongated with development of kink bands, wavy extinction and irregular margins; and the other （Fo = 96） is fine-grained and poly-angied. Some of the olivine grains contain minor Ca, Cr and Ni. Besides the exsolutions in olivine, three micron-size inclusions are also discovered. Analyzed through energy dispersive system （EDS） with unitary analytical method, the average compositions of the inclusions are： Na20, 3.12%-3.84%; MgO, 19.51%-23.79%; Al2O3, 9.33%-11.31%; SiO2, 44.89%-46.29%; CaO, 11.46%-12.90%; Cr2O3, 0.74%-2.29%; FeO, 4.26%- 5.27%, which is quite similar to those of amphibole. Diopside is anhedral f＇dling between olivines, or as micro-inclusions oriented in olivines. Chromite appears euhedral distributed between olivines, sometimes with apparent compositional zone. From core to rim of the chromite, Fe content increases and Cr decreases; and A! and Mg drop greatly on the rim. There is always incomplete magnetite zone around the chromite. Compared with the nodular chromite in the same section, the euhedral chromite has higher Fe3O4 and lower MgCr2O4 and MgAI2O4 end member contents, which means it formed under higher oxygen fugacity environment. With a geothermometer estimation, the equilibrium crystalline temperature is 820℃-960℃ for olivine and nodular chromite, 630℃-770℃ for olivine and euhedral chromite, and 350℃-550℃ for olivine and exsoluted magnetite, showing that the exsolutions occurred late at low temperature. Thus we propose that previously depleted mantle harzburgite reacted with the melt containing Na, Al and Ca, and produced an olivine solid solution added with Na^＋, Al^3＋, Ca^2＋, Fe^3＋, Cr^3＋. With temperature d 相似文献
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在吉林省南部元古宇石英岩内发现磁性微球粒３９２枚,根据其产状,形貌及一般特征,微结构和化学组成表明为陨石消融型宇宙尘,由４亚４小类组成一个宇宙尘系列,（１）金属球粒;（２）纯铁球粒,（ｂ）ＦＣＮ型（天然不锈钢）球粒;（２）氧化物球粒（ａ）普通铁质宇宙尘（ｂ）铬铁氧化物球粒;（３）玻璃质球粒;（４）氧化物－金属过渡型球粒,其母体要能是一分异的ＦＣＮ型石－铁陨石质陨星体,核部为ＦＣＮ合金,经消融分异作 相似文献
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The Effect of Postcumulus Reactions on Composition of Chrome-spinels from the Jimberlana Intrusion 总被引：2，自引：2，他引：2
Chromites in olivine adcumulates, mesocumulates and orthocumulatesfrom drill core of the Jimberlana intrusion have been analysedand related to the cumulate type and to the nature of the surroundingsilicate mineral. Chromites in adcumulates and mesocumulatesshow a restricted range of composition and are high in Mg, Aland Cr. The orthocumulate chromites vary in composition fromthat found in adcumulates to chromites which are much higherin Fe and Ti and with a higher Fe3?: Fe2? ratio. The chromitesin orthocumulates vary in composition depending upon the natureof the enclosing silicate mineral. This is believed to reflectthe ability of the enclosing mineral to protect the originalcumulus chromite from reaction with the intercumulus liquid.Thus chromite within early bronzite oikocrysts was protectedfrom reaction whereas that in plagioclase and phlogopite wasprotected at a much later stage and has a higher Fe and Ti contentChromite within olivine appears to have been able to equilibratewith intercumulus liquid until late in the magmatic historyexcept where the olivine enclosing chromite has itself beensurrounded by bronzite. It is suggested that chromite can exchangeelements with intercumulus liquid through the olivine. Thereare two possibilities; either elements such as Cr, Al, Ti andFe3 ? were able to diffuse through the olivine structure orthe apparently enclosed chromite crystals were able to maintaindirect contact with the melt along fine fractures produced bythe differential thermal contraction of olivine and chromite. The average diameters of chromite crystals within orthocumulatebronzite and olivine are 28 and 20 microns respectively whereaschromites in plagioclase and phlogopite have average diametersof 48 and 56 microns. There is no obvious correlation betweenthe size of the chromite and their composition for grains foundwithin a particular silicate. Chromites of every size have beenable to equilibrate with the liquid unless they were protectedfrom reaction. Nucleation of reaction products played an important role indetermining the final composition of any particular chromitecrystal. The significance of reaction and nucleation on a localscale of millimetres is considered with respect to the majorsilicates and to the location of the last liquid. It is suggestedthat the last liquid tended to concentrate in pockets of reactantcrystals, where product crystals failed to nucleate until latein the magmatic history. It is estimated that in rocks withan orthocumulate texture, the intercumulus liquid crystallizedover a temperature range as large as 300 ?C and that it becamesignificantly more oxidizing near the solidus temperature. 相似文献