东昆仑志留纪辉长岩地球化学特征及与铜镍成矿关系探讨

东昆仑造山带新发现的夏日哈木超大型岩浆铜镍矿床、石头坑德大型岩浆铜镍矿床及冰沟南小型岩浆铜镍矿床,其矿体均赋存于橄榄辉石岩内,而辉长岩又是该含矿橄榄辉石岩的直接围岩,并且辉长岩的形成时代相近(夏日哈木辉长岩431Ma、石头坑德辉长岩425Ma、冰沟南辉长岩427Ma),产出位置属于同一大的构造单元,均邻近昆北及昆中断裂。通过对辉长岩的地球化学特征研究,发现明显富集轻稀土元素和明显的Nb-Ta负异常,亏损高场强元素。Sr-Nd同位素研究,表明东昆仑夏日哈木和石头坑德辉长岩岩体的母岩浆来自一个曾经被交代富集的地幔源区,可能揭示了由于从洋壳释放出的流体交代地幔楔的岩石成因。结合区域构造演化和辉长岩形成时代,认为东昆仑夏日哈木和石头坑德辉长岩形成于碰撞后伸展环境。辉长岩岩浆源区性质与赋矿辉石岩存在明显不同,并非同一岩浆活动的产物。辉长岩在东昆仑造山带地区直接充当了含矿辉石岩的直接围岩,与岩浆铜镍硫化物矿体的形成没有关系,富含橄榄石的超镁铁质岩石更有利于形成具有较大经济价值的铜镍矿体。这为指导东昆仑找矿实践和岩浆铜镍矿床成矿理论研究提供了基础。     

重熔斑岩型锡多金属矿床地质特征及成矿模式

对重熔斑岩型锡多金属矿床成矿岩体的岩石类型、岩体形态、规模、岩石化学、微量元素和稀土元素地球化学、矿物包裹体和稳定同位素地球化学特征等方面进行了较系统的研究;并对该类矿床的矿化、蚀变分带特征和矿化与蚀变带的关系作了论述,指出了该类矿床最重要的蚀变带为黄玉云英岩化带, 在详细研究该类矿床的基础上,建立了重熔斑岩型锡多金属矿床的成矿模式.     

某钼-铀矿床矿化特征及成因类型探讨

矿床产于中元古代地层中。矿区内酸性脉岩发育,常密集成带,矿床受穿过脉岩带的构造破碎带控制。矿化岩石主要为构造碎裂岩和角砾岩,其原岩为长英质脉岩、变石英砂岩、变安山岩、板岩及粉砂岩等。矿化以裂隙充填为主,对围岩化学成分的选择性不大。围岩蚀变有:绢云母化、硅化、钾长石化、黑云母化、黄铁矿化、赤铁矿化及水合多水高岭石化等。铀矿物主要为沥青铀矿、铀黑、铀石,其次有钛铀矿、水铀矾,含铀矿物有锐钛矿、金红石、赤铁矿、水合多水高岭石和褐铁矿等;其它金属矿物主要有辉钼矿、黄铁矿、方铅矿和黄铜矿。矿石具脉状、角砾状、块状和浸染状构造,沥青铀矿具胶状结构。矿床中钼的储量远大于铀,铀矿体产于钼矿体之中或其边部。通过室内、外研究,可以认为本矿床为与中酸性小侵入体有关的中-低温热液成因的钼-铀型复合矿床。     

华北地台东北部前寒武纪地壳演化与铀成矿旋回

本文以研究华北地台东北部前寒武纪地壳演化为基础,阐明了该区不同地质构造单元中铀的分布与富集规律。根据铀矿化与铀源体的空间分布关系、硫同位素组成、稀上元素分布模式及同位素年龄等资料,论述了该区前寒武纪铀成矿作用具有同源性相多阶段复成因的特点。在此基础上,提出了铀成矿旋回的概念,并将华北地台东北部前寒武纪构造区存在的铀矿化划分为晚太古代、早元古代和中-晚元古代三个成矿旋回。     

中国沉积变质型铀矿床矿化特征和成矿条件探讨

我国沉积变质型铀矿床主要产在华北地台的太古界、元古界的变质岩系中,都在古老基底剥蚀面之上,有花岗岩侵入或混合岩化。古地理环境为滨海-浅海相中近古海岸线的基底洼地。矿化特点因地段不同而异:远离花岗岩地段,矿体呈似层状,与地层产状基本一致,受层位、岩性控制,铀矿物是沥青铀矿,粒度小,沿层理定向排列;近花岗岩外接触带或混合岩化地段为巢状矿体,铀矿物是晶质铀矿,粒度大,呈脉状、网脉状产出。与国外澳北区铀矿床相比,两者基本相似,但我国铀矿化分布空间大,形成时间长,无盖层。矿床形成过程为:沉积阶段形成了富铀     

陆内碰撞体制流体作用及成矿作用研究的意义和现状

陆内碰撞作用和流体作用都是８０年代以来的研究前沿，它们的研究必然会大大促进成矿作用研究的发展，也是跟踪和超越世界地球科学先进水平的重要途径。中国拥有最多最复杂的陆内碰撞带，为中国学者开发有关研究并取得高水平成果提供了得天独厚的条件。对陆内碰撞、流体作用和成矿作用研究现状的分析表明，三者之间研究的相互结合是薄弱环节，限制了有关问题的深入，但为我国学者开发该方向的研究，取得领先于国家水平的成果，提供了     

云南砂金矿床的成因类型及其找矿前景

在研究云南的残坡堆积、洪积、冲积和冰碛等砂金矿床类型的成矿作用和成矿环境的基础上,总结了云南砂金矿床地质特征。分析了砂金矿床主要受深大断裂或大断裂、地层岩石、地貌、水系和水化学环境的综合因素控制,探讨了金沙江、珠江、红河、澜沧江、怒江和伊洛瓦底江等6大水系砂金成矿条件和找矿前景预测。     

湖南宝山铜钼铅锌银多金属矿田围岩蚀变与矿化分带特征

宝山铜钼铅锌银矿田主要由中部、东部、西部和北部４个矿床组成,属岩浆期后高中温含矿热液接触交代矽卡岩型铜钼金属铋矿床、中低温热液充填交代铅锌银矿床。矿田围岩蚀变强烈,并与矿化关系密切,具有以岩体为中心向外呈现明显的围岩蚀变和矿化分带特征,可作为找矿的重要标志。     

Ages of sediment-hosted Himalayan Pb–Zn–Cu–Ag polymetallic deposits in the Lanping basin,China: Re–Os geochronology of molybdenite and Sm–Nd dating of calcite

The Lanping basin is a significant Pb–Zn–Cu–Ag mineralization belt of the Sanjiang Tethyan metallogenic province in China. Over 100 thrust-controlled, sediment-hosted, Himalayan base metal deposits have been discovered in this basin, including the largest sandstone-hosted Pb–Zn deposit in the world (Jinding), and several Cu ± Ag ± Co deposits (Baiyangping, Baiyangchang and Jinman). These deposits, with total reserves of over 16.0 Mt Pb + Zn, 0.6 Mt Cu, and 7000 t Ag, are mainly hosted in Meso-Cenozoic mottled clastic rocks, and strictly controlled by two Cenozoic thrust systems developed in the western and eastern segments of the Lanping basin.To define the metallogenic history of the study area, we dated nine calcite samples associated with copper sulfides from the Jinman Cu deposit by the Sm–Nd method and five molybdenite samples from the Liancheng Cu–Mo deposit by the Re–Os method. The calcite Sm–Nd age for the Jinman deposit (58 ± 5 Ma) and the molybdenite Re–Os age for the Liancheng deposit (48 ± 2 Ma), together with previously published chronological data, demonstrate (1) the Cu–Ag mineralization in the western Lanping basin mainly occurred in three episodes (i.e., ∼56–54, 51–48, and 31–29 Ma), corresponding to the main- and late-collisional stages of the Indo–Asian orogeny; and (2) the Pb–Zn–Ag (±Cu) mineralization in the eastern Lanping basin lacked precise and direct dating, however, the apatite fission track ages of several representative deposits (21 ± 4 Ma to 32 ± 5 Ma) may offer some constraints on the mineralization age.     

Potential martian mineral resources: Mechanisms and terrestrial analogues

The future exploration of Mars is likely to utilize resources that can be extracted in situ. An overview of the geology of Mars has been presented and several mechanisms that could result in the formation of ore deposits have been identified. These include deposits caused by hydrothermal fluids resulting from volcanic activity, large igneous province formation and impact craters. Surface enrichment of mineral sand deposits is also discussed. Where appropriate, terrestrial analogues of these mechanisms have been discussed and supporting evidence from observations of Mars undertaken to date presented. Types of deposits that are unlikely to be found on Mars are also listed.