内蒙古扎拉格阿木铜矿成矿流体与成矿机制     

车东  王建平  吴起鑫  张照志  邢恩袁  沈存利  杨文海  郭海蛟 《地质学报》2023,97(8):2575-2592

扎拉格阿木铜矿床位于锡林浩特地块北部边缘,矿体赋存于二叠纪砂质板岩和角砾岩中,受NE向断裂控制,为中温热液脉型铜矿床。本文通过流体包裹体和C?H?O?S?Pb同位素地球化学研究手段,来探讨扎拉格阿木铜矿成矿机制。成矿热液期存在5个成矿阶段：钾长石阶段、石英?绢云母阶段、石英?黄铁矿阶段、石英?多金属硫化物阶段、石英?方解石阶段。其中石英?多金属硫化物阶段为主成矿阶段,本阶段主要发育富液相、富气相、含子矿物包裹体;富液相包裹体均一温度与盐度分别为：138～289℃和2.06%～16.11% NaCl eqv;含子矿物包裹体均一温度与盐度分别为：320～374℃和32.68%～39.81% NaCl eqv,包裹体气体成分除少量CO2以外,均为H2O。H?O同位素分析表现为,石英中的〖δO〗^18值变化范围－8.5‰～7.5‰,流体的δD值变化范围为－116‰～－98‰,暗示早阶段成矿流体主要为岩浆热液,晚期伴有大气降水混入。C?O同位素分析表明,δ13C值为-6.9‰~ -10.1‰,δ18OSMOW介于2.5‰~11.7‰,在δ18O?δ13C 图上数据点落在岩浆水与大气水的中间区域。矿石硫化物的δ34S值介于-4.5‰~1.5‰,指示具有幔源岩浆硫的特征。矿石硫化物Pb同位素的208Pb/204Pb、207Pb/204Pb和206Pb/204Pb比值分别为38.034~38.609、15.497~15.655和18.141~18.446,推测Pb具有地幔来源的特点并伴有地壳或造山带Pb混入。成矿过程中伴随着流体沸腾作用,成矿物质沉淀受早期形成的岩浆热液与后加入大气降水混合的影响。  相似文献   

A critical appraisal of Sustainable Consumption and Production research: The reformist,revolutionary and reconfiguration positions     

《Global Environmental Change》2015

This conceptual review article provides a critical appraisal of Sustainable Consumption and Production research, which is currently framed by two generic positions. First, the ‘reformist’ position, which focuses on firms pursuing green eco-innovations and consumers buying eco-efficient products, represents the political and academic orthodoxy. Second, the ‘revolutionary’ position, which is a radical critique of the mainstream, advocates the abolishment of capitalism, materialism, and consumerism, and promotes values such as frugality, sufficiency, and localism. We find this dichotomous debate problematic, because it is intellectually stifling and politically conservative (in its outcomes). To move beyond this dichotomy, we propose a third position, ‘reconfiguration’, which focuses on transitions in socio-technical systems and daily life practices and accommodates new conceptual frameworks. For each of the three positions, we discuss: (1) the scale and type of change, (2) views on consumption and production in exemplary approaches, (3) underlying theoretical, epistemological and normative orientations, (4) policy implications, and (5) critical appraisal. The conclusion compares the three positions, provides arguments for the fruitfulness of the reconfiguration-position and offers four critical reflections about future Sustainable Consumption and Production research agendas.  相似文献   

基于模糊评判的数控机床零部件制造工艺FMECA研究     

谭壮  李国发  许彬彬  王松  朱光 《南京气象学院学报》2015,7(2):142-148

以数控机床零部件的制造工艺为研究对象,对其实施改进的制造工艺FMECA,通过梯形模糊数评判的方法确定出工艺FMECA中风险优先数的排序,利用模糊综合评判方法确定出工艺系统的风险等级,有效地找出薄弱工艺环节并采取改进措施,从而提高数控机床零部件制造工艺可靠性.  相似文献   

小波检验方法在国内业务模式中的最新应用研究进展     

徐同  李佳 《沙漠与绿洲气象(新疆气象)》2015,9(6):1-10

本文主要介绍小波检验方法在国内区域业务模式中的最新应用研究进展,该方法被应用于模式降水预报的个例检验和统计检验,并针对两种解决二元域限制问题的技术方案进行阐述和讨论。结果表明：D8小波可以提供一种从不同降水率阈值和空间尺度对模式定量降水预报进行评估的方案,该方案首先对预报场和分析场进行阈值获得二进制误差场,再对二进制误差场进行尺度分解,从而可以评估模式在各个降水率阈值和空间尺度上的预报技巧和偏差。统计检验结果显示模式对较大尺度降水事件表现出较高的预报技巧评分,较小尺度降水事件和强降水的预报技巧评分相对较低,并且总体上呈现出预报降水事件多于观测降水事件的特征。Padding方案和Tiling方案对应的模式统计检验结果并无明显差异,由于后者不对原始降水场做任何改变,因此是一种更为稳健和可靠的方案。  相似文献   

遥感干旱应用技术进展及面临的技术问题与发展机遇     

郭铌  王小平 《干旱气象》2015,(1):1-18

干旱是全球各地区普遍存在的一种气候现象,也是对人类社会影响最为严重的一种自然灾害。全球气候变化和社会发展加剧了干旱的影响程度,增强了干旱灾害的风险,给全球农业、水资源、生态环境安全以及社会可持续发展造成巨大威胁,提高干旱监测和早期预警技术水平是应对、管理干旱和减轻干旱脆弱性的基础。近30 a来随着全球对地观测技术的迅速发展,卫星遥感监测干旱技术取得很大进步,在全球干旱监测和早期预警中发挥着不可替代的作用。但是,干旱是多学科交叉的复杂问题,其发展过程缓慢、时间和空间表现特征差异很大,遥感监测干旱技术在应用中还存在许多技术问题,对抗旱防灾提供支撑的力度仍不够。本文在简要总结卫星遥感监测干旱应用技术的基础上,对各种指数(模型)应用中存在的问题进行评述,指出卫星遥感干旱监测面临的主要技术问题和未来发展机遇;针对我国卫星遥感干旱应用现状,提出了亟待解决的主要问题和应该努力的方向。  相似文献   

Spatially resolved spectral observations of Asteroid 951 Gaspra     

James C. Granahan 《Icarus》2011,213(1):265-272

On October 29, 1991 the Galileo spacecraft encountered Asteroid 951 Gaspra with a telescopic CCD camera and a near infrared mapping spectrometer that provided the first optically resolved views of any asteroid. Data from these two sensors were combined to detect the spectral signature of iron bearing minerals on this S-type asteroid. A minimum of two spectral units were identified on 951 Gaspra, both containing a higher relative abundance of olivine than those found in ordinary chondrites. These data indicate that this S asteroid is an object that has undergone igneous differentiation processes. A 2.7 μm spectral feature was also detected on the surface of 951 Gaspra and may be due to the presence of structural OH.  相似文献   

An in-depth look at the lunar crater Copernicus: Exposed mineralogy by high-resolution near-infrared spectroscopy     

Roberto Bugiolacchi  Urs Mall  Susan McKenna-Lawlor  Kjell Brønstad  Finn Søraas  Rolf B. Pedersen 《Icarus》2011,213(1):43-63

Newly acquired, sequentially spaced, high-resolution near-infrared spectra across the central section of crater Copernicus’ interior have been analyzed using a range of complementary techniques and indexes.We have developed a new interpretative method based on a multiple stage normalization process that appears to both confirm and expand on previous mineralogical estimations and mapping. In broad terms, the interpreted distribution of the principle mafic species suggests an overall composition of surface materials dominated by calcium-poor pyroxenes and minor olivine but with notable exceptions: the southern rim displays strong ca-rich pyroxene absorption features and five other locations, the uppermost northern crater wall, opposite rim sections facing the crater floor, and the central peak Pk1 and at the foot of Pk3, show instead strong olivine signatures.We also propose impact glass an alternative interpretation to the source of the weak but widespread olivine-like spectral signature found in low-reflectance samples, since it probably represents a major regolith constituent and component in large craters such as Copernicus.The high quality and performance of the SIR-2 data allows for the detection of diagnostic key mineral species even when investigating spectral samples with very subdued absorption features, confirming the intrinsic high-quality value of the returned data.  相似文献   

The Christiansen Effect in Saturn’s narrow dusty rings and the spectral identification of clumps in the F ring     

M.M. Hedman  P.D. Nicholson  R.H. Brown  R.N. Clark  C. Sotin 《Icarus》2011,215(2):695-711

Stellar occultations by Saturn’s rings observed with the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft reveal that dusty features such as the F ring and the ringlets in the Encke and the Laplace Gaps have distinctive infrared transmission spectra. These spectra show a narrow optical depth minimum at wavelengths around 2.87 μm. This minimum is likely due to the Christiansen Effect, a reduction in the extinction of small particles when their (complex) refractive index is close to that of the surrounding medium. Simple Mie-scattering models demonstrate that the strength of this opacity dip is sensitive to the size distribution of particles between 1 and 100 μm across. Furthermore, the spatial resolution of the occultation data is sufficient to reveal variations in the transmission spectra within and among these rings. In both the Encke Gap ringlets and F ring, the opacity dip weakens with increasing local optical depth, which is consistent with the larger particles being concentrated near the cores of these rings. The Encke Gap ringlets also show systematically weaker opacity dips than the F ring and Laplace Gap ringlet, implying that the former has a smaller fraction of grains less than ∼30 μm across. However, the strength of the opacity dip varies most dramatically within the F ring; certain compact regions of enhanced optical depth lack an opacity dip and therefore appear to have a greatly reduced fraction of grains in the few-micron size range. Such spectrally-identifiable structures probably represent a subset of the compact optically-thick clumps observed by other Cassini instruments. These variations in the ring’s particle size distribution can provide new insights into the processes of grain aggregation, disruption and transport within dusty rings. For example, the unusual spectral properties of the F-ring clumps could perhaps be ascribed to small grains adhering onto the surface of larger particles in regions of anomalously low velocity dispersion.  相似文献   

Long-term evolution of the aerosol debris cloud produced by the 2009 impact on Jupiter     

A. Sánchez-Lavega  G.S. Orton  R. Hueso  L.N. Fletcher  E. García-Melendo  I. de Pater  H.B. Hammel  A. Simon-Miller  F. Marchis  O. Mousis  J. García-Rojas  M. Cecconi  K. Noll  S. Pedraz  P. Kalas  W. Golisch  P. Sears  V. Reddy  R. Binzel  W. Grundy  J. Emery  A. Rivkin  C. Thomas  D. Trilling  K. Bjorkman  A.J. Burgasser  H. Campins  T.M. Sato  Y. Kasaba  J. Ziffer  R. Mirzoyan  H. Bouy 《Icarus》2011,214(2):462-476

We present a study of the long-term evolution of the cloud of aerosols produced in the atmosphere of Jupiter by the impact of an object on 19 July 2009 (Sánchez-Lavega, A. et al. [2010]. Astrophys. J. 715, L155-L159). The work is based on images obtained during 5 months from the impact to 31 December 2009 taken in visible continuum wavelengths and from 20 July 2009 to 28 May 2010 taken in near-infrared deep hydrogen-methane absorption bands at 2.1-2.3 μm. The impact cloud expanded zonally from ∼5000 km (July 19) to 225,000 km (29 October, about 180° in longitude), remaining meridionally localized within a latitude band from 53.5°S to 61.5°S planetographic latitude. During the first two months after its formation the site showed heterogeneous structure with 500-1000 km sized embedded spots. Later the reflectivity of the debris field became more homogeneous due to clump mergers. The cloud was mainly dispersed in longitude by the dominant zonal winds and their meridional shear, during the initial stages, localized motions may have been induced by thermal perturbation caused by the impact’s energy deposition. The tracking of individual spots within the impact cloud shows that the westward jet at 56.5°S latitude increases its eastward velocity with altitude above the tropopause by 5-10 m s⁻¹. The corresponding vertical wind shear is low, about 1 m s⁻¹ per scale height in agreement with previous thermal wind estimations. We found evidence for discrete localized meridional motions with speeds of 1-2 m s⁻¹. Two numerical models are used to simulate the observed cloud dispersion. One is a pure advection of the aerosols by the winds and their shears. The other uses the EPIC code, a nonlinear calculation of the evolution of the potential vorticity field generated by a heat pulse that simulates the impact. Both models reproduce the observed global structure of the cloud and the dominant zonal dispersion of the aerosols, but not the details of the cloud morphology. The reflectivity of the impact cloud decreased exponentially with a characteristic timescale of 15 days; we can explain this behavior with a radiative transfer model of the cloud optical depth coupled to an advection model of the cloud dispersion by the wind shears. The expected sedimentation time in the stratosphere (altitude levels 5-100 mbar) for the small aerosol particles forming the cloud is 45-200 days, thus aerosols were removed vertically over the long term following their zonal dispersion. No evidence of the cloud was detected 10 months after the impact.  相似文献   

Shoreline retreat at Titan’s Ontario Lacus and Arrakis Planitia from Cassini Imaging Science Subsystem observations   总被引：1，自引：0，他引：1  

E.P. Turtle  J.E. Perry  A.S. McEwen 《Icarus》2011,212(2):957-959

Recent observations by Cassini’s Imaging Science Subsystem reveal that part of the shoreline of Titan’s Ontario Lacus has retreated by several kilometers and may indicate that the dark area that appeared at Arrakis Planitia (80°S, 120°W) in late 2004 has subsequently faded. These changes provide constraints on aspects of Titan’s methane cycle, as well as on the properties of Titan’s surface materials.  相似文献