Evolution of Geological Environment and Its Mineralization-Controlling on Gandise Massif, Tibet, China

The Gandise massif in Tibet, China, is one of the most important copper-multimetal metallogenic belt of Tibet region( Hou, et al,2001 ; Qu, et al, 2001 ;     

基于PSInSAR方法和ASAR数据监测天津地面沉降的试验研究

概述了PSInSAR方法的技术流程，阐述了定标ENVISAT ASAR数据对PS候选点（Persistent Scatterer Cadidate，PSC）筛选 的作用。研究表明：对ENVISAR ASAR 数据进行定标有助于筛选出更多的PS候选点；以定标得到的后向散射系数作为阈值，可以剔 除散射信号统计特性较稳定但散射强度低的像素点，从而避免可能由这些点引入的相位误差。在初步实现PSInSAR方法的基础上， 运用14景ENVISAT ASAR数据获得了天津地区的年均线性沉降速率，揭示的天津市地面沉降趋势与前人研究结果较为一致，获得的形 变速率值的准确性尚待数据量的增多而进一步提高。     

辽北地区早石炭世变质火山岩年代学和地球化学特征:对华北板块北缘东段构造演化的启示

华北板块北缘东段分布的构造混杂岩带为研究古亚洲洋的演化提供了重要的依据,"下二台岩群"作为该构造混杂岩带的重要组成部分,其形成时代和构造属性仍存在争议。详细的研究表明下二台地区变质火山岩原岩包括流纹岩、英安岩、安山岩,为一套钙碱性火山岩,属于准铝质-弱过铝质岩石,根据岩相学和地球化学特征将其分为变质酸性火山岩和变质中性火山岩;二者均相对富集轻稀土元素,亏损重稀土元素,轻重稀土元素分馏明显,Eu负异常不明显,但变质中性火山岩稀土总量低于变质酸性火山岩,变质酸性火山岩明显亏损Sr、P元素,结合野外产出面积和高场强元素相关性特征,认为二者不是同一基性岩浆分异的产物。变质火山岩锆石LA-ICP-MS U-Pb年龄为341～348Ma,代表其原岩结晶年龄。变质酸性火山岩原始岩浆来自于地壳物质的部分熔融,变质中性火山岩原始岩浆来自于俯冲带附近岩石圈地幔,并遭受了地壳物质的混染,二者均形成于活动大陆边缘火山弧环境。最新研究成果表明"下二台岩群"由不同时代、不同构造环境下形成的地质单元叠置混杂而成,称其为"下二台"构造杂岩更为准确。下二台地区变质火山岩表明在早石炭世初,古亚洲洋板块已经南向俯冲,在华北板块北缘形成活动大陆边缘弧环境,早石炭世变质火山岩原岩为这一俯冲阶段的产物。     

Economic development,technological change,and the new international economic order

This paper examines dimensions of technological change and selected relationships between new technology and the process of economic development within the general framework of the New International Economic Order. Concepts discussed include economic growth and development, structural change, technological change, innovations, the transfer of technology, and appropriate technology. The relationships between these concepts are described and their significance with regard to the economic development of lesser-developed countries is assessed.     

Kimberlites: Their relation to mantle hotspots

Available age data support the hypothesis that kimberlite intrusions are formed by mantle hotspots. The hypothesis has been tested by inverting the volcanic traces formed by three hotspots to determine the post-Triassic motions of Africa, South America, and North America relative to these hotspots. Then, using these motions, the kimberlites intruded on these continents within the last 150 m.y. are relocated to their place of origin in the present hotspot reference frame. The result indicates that a majority of the kimberlites formed within 5° of a mantle hotspot. Statistical analysis shows that this kimberlite/hotspot correlation is significant at above the 90% level.     

Rare earth element distribution in some hydrothermal minerals: evidence for crystallographic control

Rare earth element (REE) abundances were measured by neutron activation analysis in anhydrite (CaSO₄), barite (BaSO₄), siderite (FeCO₃) and galena (PbS). A simple crystal-chemical model qualitatively describes the relative affinities for REE substitution in anhydrite, barite, and siderite. When normalized to ‘crustal’ abundances (as an approximation to the hydrothermal fluid REE pattern), log REE abundance is a surprisingly linear function of (ionic radius of major cation—ionic radius of REE)² for the three hydrothermal minerals, individually and collectively. An important exception, however, is Eu, which is anomalously enriched in barite and depleted in siderite relative to REE of neighboring atomic number and trivalent ionic radius. In principle, REE analyses of suitable pairs of co-existing hydrothermal minerals, combined with appropriate experimental data, could yield both the REE content and the temperature of the parental hydrothermal fluid.The REE have only very weak chalcophilic tendencies, and this is reflected by the very low abundances in galena—La, 0.6 ppb; Sm, 0.06 ppb; the remainder are below detection limits.     

Transmission electron microscope and rock magnetic investigations of remanence carriers in a Precambrian metadolerite

A Precambrian metadolerite dyke has two distinct types of remanence carriers; those with medium/high coercivities (unblocking fields of 20–120 mT) and those with low coercivities (unblocking fields of <15 mT). Optical examination reveals numerous submicron probably opaque inclusions in the plagioclase feldspar and also large opaque grains consisting of coarse oxidation-exsolution intergrowths of magnetite and ilmenite. All opaque phases have been examined using transmission electron microscopy together with microanalysis and electron diffraction. The submicron inclusions in the plagioclase are titanomagnetites(0 < x ≤ 0.14) with a size range between about 0.01 and 0.5 μm and axial ratios between 1 (equidimensional) and about 0.3. Many of these inclusions fall in the single-domain field but some are probably pseudo-single-domain. The large opaque grains contain almost pure magnetite and ilmenite and show no fine-scale exsolution; the magnetite regions of the intergrowths are of multidomain size and reveal multidomain structure under Lorentz electron microscopy. There are also some primary ilmenites containing very fine exsolved haematite, and there are very fine plates of ilmenite and very elongate needles of magnetite within the augite. Experiments on artificial samples containing very carefully prepared separates of plagioclase and large opaque grains show that the pure plagioclase acquires a remanence with unblocking fields of 20–140 mT and blocking temperatures of 390–590°C and the large opaque grains acquire a remanence with unblocking fields of less than 15 mT but a wide range of blocking temperatures up to about 570°C. It is concluded that the medium/high coercivity component of remanence in the rock is carried largely or possibly entirely by the submicron magnetites within the plagioclase and that the low coercivity component is carried largely or entirely by the multidomain magnetites in the large opaques. The contribution of the magnetite needles in the augite is uncertain as the rock does not contain any detectable component of remanence with the extremely high coercivities expected from their very elongate shape.     

Chemical fractionations in meteorites—IX. C3 chondrites

Four C3V chondrites (Grosnaja, Kaba, Mokoia, Vigarano) and three C3O chondrites (Felix, Kainsaz, and Lancé) were analyzed by radiochemical neutron activation for 17 trace elements. Both classes show a typical chondritic step pattern, reflecting loss of volatiles during chondrule formation. Elements condensing above 1300 K (U, Re, Ir, Ni) are present in essentially Cl chondrite proportions, while moderately volatile elements condensing between 1300 K and 800 K (Ge, Rb, Ag) are depleted by a factor of 0.44. However, elements condensing below 700 K (S, Cs, Bi, Tl, Br, Se, Te, In, Cd) are depleted to a still greater degree, and more so in the Ornans subclass (factor of 0.24, except Cd 0.007) than in the Vigarano subclass (factor of 0.29). This additional depletion may be due to a slight (less than 3-fold) dust-gas fractionation, by settling of dust to the median plane of the solar nebula. Among other chondrite classes, ordinary chondrites show a similar depletion, but C2 chondrites do not. Possibly the undepleted meteorites formed in one of the convection zones of the nebula predicted by Cameron and Pine, whereas the depleted meteorites formed in a quiescent region.The condensation of chalocophile elements as a function of H₂S partial pressure is discussed, in an attempt to explain the drastic difference in Cd abundance between the two subclasses. It appears that the $\text{H}{}_2\text{S}\text{H}{}_2$ ratio is the key variable. C3O's seem to have condensed in a region where enough metallic Fe was present to buffer the H₂S pressure, while C3V's condensed in a more oxidized region, where H₂S was in excess. Accretion temperatures, for an assumed nebular pressure of 10^?5 atm, were between 415 and 430 K for C3O's and less than 440 K for C3V's.Two slightly volatile elements, Sb and Au, show variable depletion, presumably reflecting variable loss during chondrule formation. Indeed, their depletion correlates with the abundance of iron-poor olivine, a measure of the peak temperature and time during chondrule formation.