Patterns of rare earth and other trace elements in different size fractions of clays of Campanian–Maastrichtian deposits from the Portuguese western margin (Aveiro and Taveiro Formations)     

Rosa Marques  M. Isabel Prudêncio  M. Isabel Dias  Fernando Rocha 《Chemie der Erde / Geochemistry》2011,71(4):337-347

The Upper Cretaceous (Campanian–Maastrichtian) Taveiro and Aveiro Formations belong to the northern sector of the Lusitanian basin (Portuguese western margin). The Taveiro Formation was deposited in alluvial fans, including mud flow beds, lakes and sinuous rivers. The Aveiro Formation was deposited in a flat region with low hydrodynamics channels, with the formation of a barrier island-tidal system. The reconstruction of this sedimentary basin may be difficult due to its complex architecture. This work aims a methodology to be used in the reconstruction of Cretaceous sedimentary environments of the Lusitanian basin, through the establishment of geochemical patterns of different size fractions of those deposits. Chemical analysis was performed by instrumental neutron activation analysis (INAA), and the mineralogical composition obtained by X-ray diffractometry (XRD). The whole rock and different size fractions (? ≥ 125 μm, 63–125 μm, 20–63 μm, 2–20 μm and ? < 2 μm) of selected samples were studied aiming the rare earth elements (REE) and other trace elements distribution and its correlation with the grain size and mineralogy.The results obtained for the studied Cretaceous sediments showed that REE patterns and other trace elements distribution in the different size fractions may be used as a tool to differentiate deposits within and between sedimentary formations. Within the Taveiro Formation, REE are concentrated in the silt fractions (20–63 μm and 2–20 μm) of the Reveles deposit, and in the clay size fraction of S. Pedro deposit, which is richer in kaolinite. The 1st transition elements, particularly Zn, are correlated with the presence of smectite in the clay fraction of Reveles deposit. In the sand and silt size fractions (>2 μm) of samples from Taveiro Formation correlations were found between: Ga and 1st transition elements, and phyllosilicates; Cs and mica; and Rb and Ba, and K–feldspars.The Bustos deposit (Aveiro Formation) samples are very fine-grained and with a high proportion of the fine silt fraction where REE are concentrated, especially the heavy ones. Incorporation of MREE, Co and U in carbonates of the coarser fraction appears to occur. The abundances of the 1st transition elements, Ga and As, are correlated with phyllosilicates.Significant differences were found in the trace elements patterns of the various analysed size fractions of the Lusitanian basin of Cretaceous sediments, between and even within formations, which can be used as a methodological approach for a fine paleogeographic reconstruction.  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   

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   

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   

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   

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   

Response of sandstone to atmospheric heating during the STONE 5 experiment: Implications for the palaeofluid record in meteorites     

John Parnell  Darren Mark 《Icarus》2008,197(1):282-290

A 1 cm thick sandstone disk exposed to atmospheric re-entry on the heat shield of a spacecraft (the STONE 5 experiment) shows alteration of fluid inclusions compared to a control sample. The sandstone contained inclusions in quartz grains, feldspar grains and calcite cement before flight. After flight, inclusions in the feldspar were all decrepitated, few inclusions in calcite survived intact and they yielded widely varying microthermometric data, and the quartz inclusions also yielded disturbed microthermometric data. The quartz becomes less affected with depth below the surface, and extrapolation suggests would be unaffected at a depth of about 2 cm. These data show that fluid inclusion data from meteorites must be treated with caution, but that a genuine fluid record may survive in the interior portions. The possibility of thermal sterilization to 2 cm depth also implies that small meteorites may be unsuitable vehicles for the transfer of microbial life from one planetary body to another. As the interiors of larger meteorites tend to have very low porosity and permeability, microbial colonization would be difficult, and the potential for panspermia is accordingly low.  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   

Intracrystalline lipids within sulfates from the Haughton Impact Structure—Implications for survival of lipids on Mars     

Stephen A. Bowden  John Parnell 《Icarus》2007,187(2):422-429

Lipids can be present within gypsum as intracrystalline inclusions if they become incorporated within the mineral as is it precipitates. The lipids that comprise these inclusions are protected against alteration or destruction by an external oxidising chemical environment because a protective mineral matrix surrounds them. Sulfate minerals are abundant on the surface of Mars and were present in the samples that were analysed by the Viking landers. The quantities of secondary intracrystalline fossil-lipids that are present in samples of gypsum and gypsum-rich soils from the Haughton Impact Structure, Devon Island, Canadian High Arctic are sufficient to suggest that if a similar concentration of fossil lipids was present in the sulfate-rich samples analysed by the Viking Landers then they could have been detected. Possible reasons why a secondary fossil-lipid signature was not detected include a poor rate of conversion during pyrolysis, exposure of intracrystalline lipids during periods of weathering to oxidative martian diagenesis, a low level of biological productivity or an absence of a source for lipids on the surface of Mars. Polycyclic aromatic hydrocarbons of meteoritic origin, and terpane biomarkers such as hopanes and steranes, are not present in the Haughton gypsum in sufficient quantities to have been readily detected.  相似文献   

Evidence for enhanced hydration on the northern flank of Olympus Mons, Mars     

Giancarlo Bellucci  Joern Helbert  Francesca Altieri  Dennis Reiss  Jean-Pierre Bibring  Stephan van Gasselt  Harald Hoffmann  Yves Langevin  Gerhard Neukum  Franois Poulet 《Icarus》2007,192(2):361-377

In this paper we report about a small region on the northern scarp of Olympus Mons showing an increase of the 3 μm hydration band in the OMEGA spectra, together with low superficial temperatures. Although water ice clouds can occurs on the flank of big martian volcanoes, radiative transfer modeling indicates that atmospheric water ice alone cannot justify the shape of the observed band. A fit of the 1.9–3 μm absorption features is obtained by hypothesizing that the study region consists of a mixture of dust and water ice covered by an optically thin (τ=0.08 at 3 μm) layer of dust. Thermal modeling also suggests that water ice in this region may be stable during most of the martian year due to the saturation of the atmosphere. If water ice is responsible for the observed spectral behavior, it might consist of a number of ice or snow patches possibly deposited in small depressions.  相似文献