东坪式与正长岩类有关的金矿床成矿机理的同位素地球化学制约     

包志伟  赵振华 《岩石学报》2006,22(10):2534-2542

东坪式金矿床产于华北地台北缘金矿成矿带的冀西北金矿集中区,构造上位于华北克拉通北缘深大断裂-尚义-赤城断裂的南侧。金矿床产于泥盆纪早期(386～410Ma)水泉沟正长岩杂岩体内及接触带附近,矿体分布受脆-韧性剪切断裂构造的制约。金矿成矿作用具有多期次的特点,成矿时代为燕山期(156～203Ma)。矿石类型主要为石英脉型、石英网脉 脉旁钾硅化蚀变岩型和钾硅化蚀变岩型,具有典型的碱性岩金矿的金-碲组合,(含)金矿物主要为自然金、碲金矿和碲金银矿。流体包裹体的 H、O 及 He 同位素研究表明,成矿流体为以大气降水主的混合热液流体并可能存在深源流体的参与。矿床的 S、Pb、Sr 和 Si 同位素组成表明,金矿成矿物质主要来源于正长岩杂岩体,部分源于太古宙桑干群变质岩和燕山期花岗岩。因此,东坪式金矿是由燕山期伸展构造环境下热液流体在上涌地幔及岩浆活动的热驱动下对泥盆纪早期形成的正长岩交代改造的产物。  相似文献   

中国海相碳酸盐岩层系油气地质特点、战略选区思考及需要解决的主要地质问题   总被引：2，自引：0，他引：2  

汤良杰  吕修祥  金之钧  刘小平  邱楠生 《地质通报》2006,(Z2)

中国海相碳酸盐岩层系油气资源量大,但探明程度低,是油气资源战略接替的重要领域。中国海相碳酸盐岩层系具有形成时代老、改造强烈、沉积中心与生烃中心不吻合、储层具有多样性且非均质性强、多烃源层、多期生烃、多期成藏、多期调整与改造等显著特点,与陆相碎屑岩层系有明显差别,又有别于国外海相碳酸盐岩层系。在对不同地区海相碳酸盐岩层系油气地质条件进行分析解剖的基础上,分别对四川盆地、中下扬子及滇黔桂地区、塔里木盆地、鄂尔多斯盆地、渤海湾盆地和青藏地区的海相碳酸盐岩层系油气勘探战略选区急需解决的地质问题进行了讨论。  相似文献   

陕西凤县八方山-二里河（铜）铅锌矿床地质特征及成矿模式     

陈二虎张新胜  高卫宏 《西北地质》2007,40(B07):13-17

在综合分析凤-太矿集区成矿构造特征的基础上，依据以往总结的凤．太矿田铅锌、金矿聚矿构造模式，通过对八方山-二里河铅锌矿床地质特征的分析，总结了找矿标志，初步认为八方山-二里河（铜）铅锌矿床的成矿模式为：“前泥盆纪海底热水喷流沉积一印支-燕山期构造改造型”铅锌矿床。认为成矿物质来源于基底，后期的构造-岩浆改造使基底成矿元素活化，沿同生断裂迁移、改造，最后在泥盆系中形成的扩容性构造部位富集成矿。提出了下一步扩大找矿的方向和建议。  相似文献   

ENVIRONMENTAL MIGRATION AND SUSTAINABLE DEVELOPMENT——A Case Study of Southwest China     

王克林 《中国地理科学(英文版)》1998,(3)

Ｉ．ＩＮＴＲＯＤＵＣＴＩＯＮＩｔｉｓｇｅｎｅｒａｌｙａｃｃｅｐｔｅｄｔｈａｔｔｈｅｄｅｇｒａｄａｔｉｏｎｏｆｒｅｎｅｗａｂｌｅｒｅｓｏｕｒｃｅｓａｎｄｆｒａｇｉｌｅｅｎｖｉｒｏｎｍｅｎｔｓｉｎｄｅｖｅｌｏｐｉｎｇｃｏｕｎｔｒｉｅｓｉｓｂｅｃｏｍｉｎ...  相似文献   

苏北超基性岩某些超高压变质特征   总被引：10，自引：2，他引：8  

陆永增 《江苏地质》1998,22(1):1-9

苏北芝麻坊超基性岩体,位于大别—苏鲁超高压变质带东段的核心部位,与基性榴辉岩紧密伴生,是苏北最具代表性的岩体之一。根据多年来的成果资料,研究它的超高压变质特征,对研究整个苏鲁超高压变质带具有重大意义。对岩体的形态特征、岩相学特征、特别是矿物学特征,如镁铝榴石特征的研究,结合金刚石的选出,都有力的证实苏北超基性岩是在超高压变质环境下生成的,同时也反映其是由华北地块与扬子地块俯冲碰撞而从地壳深处挤压上来的幔源物质。  相似文献   

爆炸影响降水的观测分析   总被引：1，自引：0，他引：1  

大气物理研究所三室原理组 《大气科学》1976,(1):62-67

本文对“炮响雨落”的现象进行了实验验证。初步结果表明:在一定云雨条件下,炮击后可能促使未降水积状云产生降水,也可能促使已降水云的降水参量增大,这些变化发生迅速,但维持时间不长。并指出炮击促进云体降水的作用可能是通过改变支托水滴的气流造成的。在适当条件下,通过炮击影响气流的瞬时作用,可能触发云内不稳定能量释放,造成持续下沉,破坏云的发展,从而防止冰雹灾害。  相似文献   

夏季青藏高原流场三维结构的模拟实验     

中国科学院大气物理研究所二室模拟组 《大气科学》1977,1(4):247-255

本文用流体模拟实验的方法,研究了我国夏季青藏高原及邻近地区环流的三维结构和成因,主要结果为: 无转动因素时,高原加热作用能引起流体在低层径向地朝高原辐合,在高原上层放射状向周围辐散.高层辐散流体的一部分在高原内部开始下沉,形成高原上空的对流环,在有转动的实验中也观察到.辐散流体中还出现波动. 高原内部经常出现两个对流上升中心,中心附近的温度有较大脉动,两个对流上升区之间有时为下沉运动,构成高原内部独特的对流环. 通过高原中部的南北垂直剖面上,可观察到方向相反的两个对流环,流体在高原中部上升,在南北高原范围内下沉.在高原外部为高原加热引起的下沉运动. 实验表明,包括基本东西风和高原以外热源的环境背景条件,对高原流场有重要作用. 实验结果为解决夏季青藏高原环流的三维结构提供了依据,文中列举了一些说明的现象。  相似文献   

l0舰船科学技术Ship Science and     

Technology 《国土资源导刊(湖南)》2007,(11)

青岛266071潜艇;;定深旋回;;控制定深等速直航潜艇操方向舵后将逐渐进入并保持圆周运动,要实现潜艇定深旋回,可同时操纵尾升降舵、首升降舵或者首尾升降舵配合操舵。通过仿真分析各种操纵方案的优劣,得到实现定深旋回的最佳控制方式。Modeling and analysis on the control of submarine's certain depth and gyration motionCHEN Jun-feng, TIAN Wei,CHE Meng-hu (Navy Submarine Academy, Qingdao 266071, China)Submarine will go into and keep the states of circular motion under the contro  相似文献   

Characteristics of convection and overshooting in RGB and AGB stars     

Xiang-Jun Lai    Yan Li  National Astronomical Observatories/ Yunnan Observatory  Chinese Academy of Sciences  Kunming  China  Key Laboratory for the Structure  Evolution of Celestial Objects  China Graduate University of Chinese Academy of Sciences  Beijing  China. 《中国天文和天体物理学报》2011,(10)

Based on the turbulent convection model (TCM) of Li & Yang, we have studied the characteristics of turbulent convection in the envelopes of 2 and 5M⊙ stars at the red giant branch and asymptotic giant branch phases. The TCM has been successfully applied over the entire convective envelopes, including the convective unstable zone and the overshooting regions. We find that the convective motions become progressively stronger when the stellar models are located farther up along the Hayashi line. In the convect...  相似文献   

Cassini SAR, radiometry, scatterometry and altimetry observations of Titan’s dune fields     

A. Le Gall  M.A. Janssen  A.G. Hayes  C. Savage  R.D. Lorenz  R.L. Kirk  S. Wall  E.R. Stofan  the Cassini Radar Team 《Icarus》2011,213(2):608-624

Large expanses of linear dunes cover Titan’s equatorial regions. As the Cassini mission continues, more dune fields are becoming unveiled and examined by the microwave radar in all its modes of operation (SAR, radiometry, scatterometry, altimetry) and with an increasing variety of observational geometries. In this paper, we report on Cassini’s radar instrument observations of the dune fields mapped through May 2009 and present our key findings in terms of Titan’s geology and climate. We estimate that dune fields cover ∼12.5% of Titan’s surface, which corresponds to an area of ∼10 million km², roughly the area of the United States. If dune sand-sized particles are mainly composed of solid organics as suggested by VIMS observations (Cassini Visual and Infrared Mapping Spectrometer) and atmospheric modeling and supported by radiometry data, dune fields are the largest known organic reservoir on Titan. Dune regions are, with the exception of the polar lakes and seas, the least reflective and most emissive features on this moon. Interestingly, we also find a latitudinal dependence in the dune field microwave properties: up to a latitude of ∼11°, dune fields tend to become less emissive and brighter as one moves northward. Above ∼11° this trend is reversed. The microwave signatures of the dune regions are thought to be primarily controlled by the interdune proportion (relative to that of the dune), roughness and degree of sand cover. In agreement with radiometry and scatterometry observations, SAR images suggest that the fraction of interdunes increases northward up to a latitude of ∼14°. In general, scattering from the subsurface (volume scattering and surface scattering from buried interfaces) makes interdunal regions brighter than the dunes. The observed latitudinal trend may therefore also be partially caused by a gradual thinning of the interdunal sand cover or surrounding sand sheets to the north, thus allowing wave penetration in the underlying substrate. Altimetry measurements over dunes have highlighted a region located in the Fensal dune field (∼5° latitude) where the icy bedrock of Titan is likely exposed within smooth interdune areas. The hemispherical assymetry of dune field properties may point to a general reduction in the availability of sediments and/or an increase in the ground humidity toward the north, which could be related to Titan’s asymmetric seasonal polar insolation. Alternatively, it may indicate that either the wind pattern or the topography is less favorable for dune formation in Titan’s northern tropics.  相似文献