Mineralogical and geochemical investigations of the Dajia Salento-type bauxite deposits,western Guangxi,China     

Xuefei Liu  Qingfei Wang  Jun Deng  Qizuan Zhang  Silei Sun  Jianyin Meng 《Journal of Geochemical Exploration》2010

The Dajia Salento-type bauxite deposit in western Guangxi is hosted within the Quaternary ferrallitic soil profile, and it formed via breaking up, weathering and oxidizing of Permian bauxite orebodies occurring as a semi-continuous layer in the upper Permian. Mineralogical analyses reveal that diaspore, hematite and kaolinite are the major minerals in bauxite ores with small amounts of anatase, chamosite, gibbsite, goethite, illite, zircon, quartz and pyrite. The ore texture and mineral assemblage reveal that the depositional/diagenetic environment of the Dajia bauxite was much close to phreatic environment. Both the ore texture and the morphology of zircon grains also indicate that most of the bauxitic soils were transported a short distance. Diaspore is suggested to be non-metamorphic in origin and mainly formed in a reducing condition of diagenetic environment, while kaolinite is the product of the in situ epigenetic replacement of alumina in diaspore by dissolved silica. Geochemical analyses indicate that Al₂O₃, Fe₂O₃, SiO₂ and TiO₂ are the main components of the bauxite ores and trace elements such as Zr, Hf, Nb, Ta, Th and U were enriched during the bauxitization process. Simultaneously, Zr vs. Hf and Nb vs. Ta show a high correlation. Geochemical indices such as Zr/Hf, Nb/Ta and Eu/Eu* (among others) denote that the magmatic rocks related to the Emeishan plume in western Guangxi and the carbonates in the underlying Maokou Formation provided the main sources of material for the bauxite ores.  相似文献   

中亚萨亚克矿田成矿岩体矿物学和地球化学:岩浆性质与成矿意义   总被引：3，自引：1，他引：2  

安芳  王居里  朱永峰  王建其  魏少妮  赖绍聪  SEITMURATOVA Eleonora 《岩石学报》2015,31(2):555-570

萨亚克大型铜矿田位于哈萨克斯坦北巴尔喀什斑岩成矿带中部,以矽卡岩型矿床为主。通过对矿区石英闪长岩的矿物化学和地球化学研究,发现石英闪长岩呈斑状结构,斑晶为斜长石和角闪石,其中的斜长石斑晶主要为中长石,角闪石斑晶为镁质普通角闪石;岩石属于高钾钙碱性系列,富集Rb、Sr、Ba等大离子亲石元素和轻稀土元素,亏损Nb、Ta和重稀土元素,高Sr/Y、La/Yb比值,与埃达克岩相似。地球化学特征指示萨亚克矿区侵入岩形成于岛弧环境,为矽卡岩-斑岩型成矿提供了有利的构造背景,岩石可能是岛弧玄武质岩浆在高压下经结晶分异而成。根据角闪石温压计及其成分与氧逸度和岩浆中水含量之间的关系,确定萨亚克石英闪长玢岩中角闪石斑晶结晶时岩浆的温度为799~843℃、处于3.6~9.6km深度范围内(P=1.2~3.2kbar)、氧逸度logfO2=-11.5~-12.0(ΔFMQ=2.0~2.8)、平均水含量为1.2%,相对较高的氧逸度和水含量有利于形成富含挥发分和Cu、Au等成矿物质的岩浆,是最终演化形成大型岩浆-热液型铜矿田(斑岩型、矽卡岩型)的有利条件。  相似文献   

胶北地块变质基底超镁铁岩的矿物岩石地球化学特征   总被引：2，自引：2，他引：0  

孔凡梅  刘云  李旭平  郭敬辉  赵国春 《岩石学报》2015,31(6):1549-1563

胶北地块变质基底的蛇纹岩、蛇纹岩化尖晶石方辉橄榄岩、尖晶石橄榄斜方辉石岩、角闪石岩自形成以后,经历了早期的高角闪岩相和晚期绿片岩相的变质作用,因而记录了三个阶段的矿物组合:早期的Opx1+Ol1+Spl1;中期的Opx2+Ol2+Spl2+Amp2和晚期的Amp3+Srp3+Mag3+Cal组合。超镁铁岩中普遍存在的角闪石,具有粒状变晶结构特征,形成于角闪岩相和绿片岩相的变质作用过程。蛇纹石没有受到应力作用的迹象,显示其形成于晚期非挤压环境的交代变质作用过程。尖晶石橄榄岩中斜方辉石的矿物化学以及尖晶石橄榄岩的高Mg O含量都表现出克拉通橄榄岩的性质。角闪石岩的稀土元素配分图解的(La/Sm)N的比值1.11~1.41,(La/Yb)N的比值0.91~1.61,超镁铁岩多元素图解显示无高场强元素异常,都表明胶北地块变质基底的超镁铁岩形成的构造背景或是裂谷环境。尖晶石矿物的Mg#0.72~0.79、Cr#0.06~0.12表明交代变质成因。方辉橄榄岩橄榄石的Fo值88.42~90.50、超镁铁质岩石全岩主元素的分散性、较大的∑REE含量变化以及Si/Al-(Mg+Fe)/Al和Mg/Ti-Fe/Ti主元素的比值图解所表现出的超镁铁岩与角闪石岩具有成因联系等,都表明胶北变质基底的超镁铁岩可能是具有堆晶成因的一套幔源岩浆系列。高MgO含量(16%~42%)表现出前寒武纪变质基底的橄榄岩地幔性质;高水含量反映出漫长地质历史时期变质作用过程。  相似文献   

荷叶塘陨石:一个L3型普通球粒陨石的岩石学和地球化学特征     

王桂琴  缪秉魁  林杨挺 《岩石学报》2015,31(9):2724-2736

荷叶塘为一块我国降落的原始3型普通球粒陨石,因此具有重要研究意义。本文对荷叶塘陨石光薄片及粉末样品的岩石学、矿物学和全岩组成地球化学特征进行研究,为这块陨石的深入研究提供重要基础数据。研究表明荷叶塘陨石具L3型陨石岩石学特征,具典型的球粒陨石结构,球粒清晰,球粒结构类型多,基质重结晶程度低,组成模式为:球粒80vol%,金属和硫化物含量为5vol%,基质15vol%。矿物化学成分表明,该陨石球粒以Ⅰ型(贫铁型)球粒为主,橄榄石Fa0.41-34.1(PMD=51),低钙辉石Fs1.82-27.2(PMD=88),Wo0.18-3.13(PMD=103),铁纹石中Co含量平均0.62%(PMD=20),矿物成份不均一程度高,橄榄石矿物结晶颗粒内部化学成分变化大,呈正环带分布,与岩浆型结晶顺序一致,球粒与基质及间隙物成分明显不同,表现为不同物质来源。化学成分全岩分析结果显示,荷叶塘陨石亲石、亲铁元素含量均为L型陨石特征。依据以上岩石矿物学和化学组成特征,依照陨石亚分类参数,将其类型划分为L3.4型普通球粒陨石。冲击变质程度S2,风化程度W1。研究结果表明荷叶塘陨石为一块受后期水、热蚀变和风化影响较少的原始类型陨石。组成矿物成分极不均一,在矿物晶体内部,球粒内部及球粒与基质间均有明显变化。  相似文献   

西南三江普朗铜矿岩浆混合作用:矿物学和地球化学证据   总被引：3，自引：2，他引：1  

刘欢  张长青  贾福东  周云满  娄德波 《岩石学报》2015,31(11):3189-3202

岩浆混合作用是近年来岩石学研究中的热点与难点,其研究对揭示壳幔相互作用,探讨成岩成矿过程具有重要意义。普朗铜矿位于西南三江义敦岛弧南段,是我国近年来发现的超大型斑岩铜矿床。矿体产于复式岩体中,复式岩体内发育大量暗色微粒包体。包体粒度较细,多呈椭圆形,其内可见具暗色矿物镶边的眼球状石英、针状磷灰石以及具有结构与成分不平衡现象的斜长石斑晶;与寄主岩相比,包体富集黑云母、角闪石等暗色矿物。主量元素组成上,包体相对于寄主岩Si O2(53.67%~61.50%)含量较低,Mg O(3.12%~5.40%)和Fe2OT3(3.38%~9.00%)含量较高。微量元素结果显示,包体与寄主岩具有相似的微量元素组成与稀土元素配分模式,均表现为富集大离子亲石元素(K、Rb、Ba、Sr),亏损高场强元素(Nb、Hf、P、Ti),无明显的δCe异常,轻稀土元素富集,重稀土元素亏损;但与寄主岩相比,包体具有较高的稀土元素总量(119.0×10-6~308.9×10-6)与较明显的Eu负异常(δEu=0.56~0.95)。以上结果表明,包体为岩浆混合作用的产物。文章进一步采用多重分形理论解析了包体中Mg、Fe、Ca、Al、K、Ti、P及Ba等元素的分布特征,定量刻画了岩浆混合作用的程度。结果表明,元素分布的多重分形谱越宽,关联维越小,则岩浆混合程度越高。  相似文献   

Blowing in the wind. II. Creation and redistribution of refractory inclusions in a turbulent protoplanetary nebula     

Jeffrey N. Cuzzi  Sanford S. Davis  Anthony R. Dobrovolskis 《Icarus》2003,166(2):385-402

Ca-Al rich refractory mineral inclusions (CAIs) found at 1-6% mass fraction in primitive chondrites appear to be 1-3 million years older than the dominant (chondrule) components which were accreted into the same parent bodies. A prevalent concern is that it is difficult to retain CAIs for this long against gas-drag-induced radial drift into the Sun. We reassess the situation in terms of a hot inner (turbulent) nebula context for CAI formation, using analytical models of nebula evolution and particle diffusion. We show that outward radial diffusion in a weakly turbulent nebula can overcome inward drift, and prevent significant numbers of CAI-size particles from being lost into the Sun for times on the order of 10⁶ years. CAIs can form early, when the inner nebula was hot, and persist in sufficient abundance to be incorporated into primitive planetesimals at a much later time. Small (?0.1 mm diameter) CAIs persist for longer times than large (?5 mm diameter) ones. To obtain a quantitative match to the observed volume fractions of CAIs in chondrites, another process must be allowed for: a substantial enhancement of the inner hot nebula in silicate-forming material, which we suggest was caused by rapid inward drift of meter-sized objects. This early in nebula history, the drifting rubble would have a carbon content probably an order of magnitude larger than even the most primitive (CI) carbonaceous chondrites. Abundant carbon in the evaporating material would help keep the nebula oxygen fugacity low, plausibly solar, as inferred for the formation environment of CAIs. The associated production of a larger than canonical amount of CO₂ might also play a role in mass-independent fractionation of oxygen isotopes, leaving the gas rich in ¹⁶O as inferred from CAIs and other high temperature condensates.  相似文献   

Light-toned layered deposits in Juventae Chasma, Mars     

David C. Catling  Stephen E. Wood  David R. Montgomery  Christopher R. Glein 《Icarus》2006,181(1):26-51

We examine hypotheses for the formation of light-toned layered deposits in Juventae Chasma using a combination of data from Mars Global Surveyor's Mars Orbiter Camera (MOC), Mars Orbiter Laser Altimeter (MOLA), and Thermal Emission Spectrometer (TES), as well as Mars Odyssey's Thermal Emission Imaging System (THEMIS). We divide Juventae Chasma into geomorphic units of (i) chasm wall rock, (ii) heavily cratered hummocky terrain, (iii) a mobile and largely crater-free sand sheet on the chasm floor, (iv) light-toned layered outcrop (LLO) material, and (v) chaotic terrain. Using surface temperatures derived from THEMIS infrared data and slopes from MOLA, we derive maps of thermal inertia, which are consistent with the geomorphic units that we identify. LLO thermal inertias range from ∼400 to 850 J m⁻² K⁻¹ s^−1/2. Light-toned layered outcrops are distributed over a remarkably wide elevation range () from the chasm floor to the adjacent plateau surface. Geomorphic features, the absence of small craters, and high thermal inertia show that the LLOs are composed of sedimentary rock that is eroding relatively rapidly in the present epoch. We also present evidence for exhumation of LLO material from the west wall of the chasm, within chaotic and hummocky terrains, and within a small depression in the adjacent plateau. The data imply that at least some of the LLO material was deposited long before the adjacent Hesperian plateau basalts, and that Juventae Chasma underwent, and may still be undergoing, enlargement along its west wall due to wall rock collapse, chaotic terrain evolution, and exposure and removal of LLO material. The new data allow us to reassess possible origins of the LLOs. Gypsum, one of the minerals reported elsewhere as found in Juventae Chasma LLO material, forms only at low temperatures () and thus excludes a volcanic origin. Instead, the data are consistent with either multiple occurrences of lacustrine or airfall deposition over an extended period of time prior to emplacement of Hesperian lava flows on the plateau above the chasm.  相似文献   

Water sorption on martian regolith analogs: Thermodynamics and near-infrared reflectance spectroscopy     

Antoine Pommerol  Bernard Schmitt  Pierre Beck  Olivier Brissaud 《Icarus》2009,204(1):114-136

The near-infrared reflectance spectra of the martian surface present strong absorption features attributed to hydration water present in the regolith. In order to characterize the relationships between this water and atmospheric vapor and decipher the physical state of water molecules in martian regolith analogs, we designed and built an experimental setup to measure near-IR reflectance spectra under martian atmospheric conditions. Six samples were studied that cover part of the diversity of Mars surface mineralogy: a hydrated ferric oxide (ferrihydrite), two igneous samples (volcanic tuff, and dunite sand), and three potential water rich soil materials (Mg-sulfate, smectite powder and a palagonitic soil, the JSC Mars-1 regolith stimulant). Sorption and desorption isotherms were measured at 243 K for water vapor pressure varying from 10⁻⁵ to ∼0.3 mbar (relative humidity: 10⁻⁴ to 75%). These measurements reveal a large diversity of behavior among the sample suite in terms of absolute amount of water adsorbed, shape of the isotherm and hysteresis between the adsorption and desorption branches. Simultaneous in situ spectroscopic observations permit a detailed analysis of the spectral signature of adsorbed water and also point to clear differences between the samples. Ferric (oxy)hydroxides like ferrihydrite or other phases present in palagonitic soils are very strong water adsorbent and may play an important role in the current martian water cycle by allowing large exchange of water between dust-covered regions and atmosphere at diurnal and seasonal scales.  相似文献   

Spectral and geological study of the sulfate-rich region of West Candor Chasma, Mars     

Nicolas Mangold  Aline Gendrin  Stephane LeMouelic  Véronique Ansan  Yves Langevin  Gerhard Neukum 《Icarus》2008,194(2):519-543

Sulfates have been discovered by the OMEGA spectrometer in different locations of the planet Mars. They are strongly correlated to light toned layered deposits in the equatorial regions. West Candor Chasma is the canyon with the thickest stack of layers and one with the largest area covered by sulfates. A detailed study coupling mineralogy derived from OMEGA spectral data and geology derived from HRSC imager and other datasets leads to some straightforward issues. The monohydrated sulfate kieserite is found mainly over heavily eroded scarps of light toned material. It likely corresponds to a mineral present in the initial rock formed either during formation and diagenesis of sediments, or during hydrothermal alteration at depth, because it is typically found on outcrops that are eroded and steep. Polyhydrated sulfates, that match any Ca-, Na-, Fe-, or Mg-sulfates with more than one water molecule, are preferentially present on less eroded and darker outcrops than outcrops of kieserite. These variations can be the result of a diversity in the composition and/or of the rehydration of kieserite on surfaces with longer exposure. The latter possibility of rehydration in the current, or recent, atmosphere suggests the low surface temperatures preserve sulfates from desiccation, and, also can rehydrate part of them. Strong signatures of iron oxides are present on sulfate-rich scarps and at the base of layered deposits scarps. They are correlated with TES gray hematite signature and might correspond to iron oxides present in the rock as sand-size grains, or possibly larger concretions, that are eroded and transported down by gravity at the base of the scarp. Pyroxenes are present mainly on sand dunes in the low lying terrains. Pyroxene is strongly depleted or absent in the layered deposits. When mixed with kieserite, local observations favor a spatial mixing with dunes over layered deposits. Sulfates such as those detected in the studied area require the presence of liquid water to form by precipitation, either in an intermittent lacustrine environment or by hydrothermal fluid circulation. Both possibilities require the presence of sulfur-rich groundwater to explain fluid circulation. The elevation of the uppermost sulfate signatures suggests the presence of aquifers up to 2.5 km above datum, only 1 km below the plateau surface.  相似文献   

Generation and performance of automated jarosite mineral detectors for visible/near-infrared spectrometers at Mars   总被引：1，自引：0，他引：1  

Martha S. Gilmore  Benjamin Bornstein  Rebecca Castaño 《Icarus》2008,195(1):169-183

We have developed two automated detectors that can recognize the sulfate mineral jarosite in unknown visible to near-infrared spectra (350-2500 nm). The two detectors are optimized for use within the terrestrial and martian atmospheres. The detectors are built from Support Vector Machines trained using a generative model to create linear mixtures of library mineral spectra. Both detectors performed with an average ∼90% accuracy on laboratory spectra of single minerals and the laboratory and field spectra of rocks collected in a hydrothermal environment. This type of algorithm will contribute to the efficiency of onboard data analysis of landed and orbital visible/near-infrared spectrometers at Mars.  相似文献