玛曲县格尔柯金矿床控矿地质条件及其矿床成因探讨

格尔柯金矿 (即大水金矿 )是产于西秦岭南带西倾山—迭山逆冲褶断带南缘的特大型金矿。矿床控矿地质条件为构造单元界断裂带、深源浅成花岗闪长斑岩小侵入体、下三叠统马热松多组 (T1m)碳酸盐岩沉积建造 ,与金矿关系密切的矿化蚀变有硅化、赤铁矿化、褐铁矿化和方解石化 ;矿床成因类型为层控—热水溶滤构造蚀变岩型。     

赣北主要内生金矿床的形成条件

赣北地区的金矿床,可分为含金韧性剪切带型、硅化破碎带型、隐爆角砾岩型和微细粒浸染型等4个类型,其原始成矿物质来源于上地幔,通过火山喷发—沉积作用,形成含金沉积建造和含金火山岩建造.钠、钾质两个系列的花岗质岩石都可以形成金矿床.矿化富集主要通过韧、脆性变形和岩浆隐蔽爆破,产生多次破碎,多期蚀变矿化.在中—低温热液阶段,含矿热液体系的HS~-、Cl~-离子减少,还原介质增加的条件下沉淀富集,形成不同类型的金矿床.     

云南宝兴厂金多金属矿床成矿地质条件

矿区金、铜、钼矿化与碱性斑岩相关,向阳组碎屑岩是主要矿源层及赋矿地层,北东向响水断裂控矿,近东西向次级断裂及层间断裂为储（容）矿构造。多种条件耦合成矿。     

Thermal contraction crack polygons on Mars: A synthesis from HiRISE, Phoenix, and terrestrial analog studies

Thermal contraction crack polygons are complex landforms that have begun to be deciphered on Earth and Mars by the combined investigative efforts of geomorphology, environmental monitoring, physical models, paleoclimate reconstruction, and geochemistry. Thermal contraction crack polygons are excellent indicators of the current or past presence of ground ice, ranging in ice content from weakly cemented soils to debris-covered massive ice. Relative to larger topographic features, polygons may form rapidly, and reflect climate conditions at the time of formation—preserving climate information as relict landforms in the geological record. Polygon morphology and internal textural characteristics can be used to distinguish surfaces modified by the seasonal presence of a wet active layer or dry active layer, and to delimit subsurface ice conditions. Analysis of martian polygon morphology and distribution indicates that geologically-recent thermal contraction crack polygons on Mars form predominantly in an ice-rich latitude-dependent mantle, more likely composed of massive ice deposited by precipitation than by cyclical vapor diffusion into regolith. Regional and local heterogeneities in polygon morphology can be used to distinguish variations in ice content, deposition and modification history, and to assess microclimate variation on timescales of ka to Ma. Analyses of martian polygon morphology, guided by investigations of terrestrial analog thermal contraction crack polygons, strongly suggest the importance of excess ice in the formation and development of many martian thermal contraction crack polygons—implying the presence of an ice-rich substrate that was fractured during and subsequent to obliquity-driven depositional periods and continually modified by ongoing vapor equilibration processes.     

新疆西昆仑奥尔托喀讷什锰矿地质、地球化学及成因

近年来,西昆仑玛尔坎苏地区富锰矿找矿取得重大突破,新发现奥尔托喀纳什等大型锰矿床。该矿床层位稳定,厚度较大,Mn平均品位达35%以上,为中国最富的碳酸锰矿床,属于典型的海相沉积型锰矿床。锰矿体主要赋存于晚石炭世喀拉阿特河组地层中,该组岩性为一套浅海碳酸盐岩台地相沉积建造组合,可划分为台内浅滩、潮坪、开阔台地、局限台地等4个相类型。成矿分为三个期次,第一期为沉积成岩成矿期,矿石矿物由菱锰矿、锰方解石、硼锰矿组成;第二期为热液改造期,形成锰镁绿泥石、红锰矿、硫锰矿、锰方解石(脉)、重结晶菱锰矿、蔷薇辉石及滑石、石膏等;第三期为表生氧化期,发育少量软锰矿、水锰矿、硬锰矿等。锰矿石具有较低的Fe/Mn比值、V/(V+Ni)比值和强烈的Ce正异常,表明Mn是在氧化环境下,以氧化物或氢氧化物的形式沉积富集。含锰岩系顶、底板岩石中含较多成熟度较差的中酸性火山岩岩屑,以及具有较低Al/(Al+Fe+Mn)、Y/Ho、Co/Ni比值的锰矿石,说明其成矿物质来源于海底热水活动。奥尔托喀纳什锰矿具有"内源外生"的特点,锰矿石及菱锰矿具有负的δ~(13)C值(-23.3‰～-13.2‰),表明锰矿经历了先成锰氧化物或氢氧化物、再被还原转化成菱锰矿的过程。此外,有机质所导致的更为强烈的还原作用是本矿床富锰矿形成的重要机制。后期构造叠加致使矿体发生变形,矿体形态受褶皱控制。矿石受到强烈改造,形成锰镁绿泥石、红锰矿、蔷薇辉石等,晚期经历氧化淋滤作用形成软锰矿、水锰矿等。     

Geochemical Characteristics and Genetic Significance of Datangpo‐Type Manganese Ore Deposits during the Cryogenian Period

The Datangpo‐type manganese ore deposits, which formed during the Nanhuan (Cryogenian) period and are located in northeastern Guizhou and adjacent areas, are one of the most important manganese resources in China, showing good prospecting potential. Many middle‐to‐large deposits, and even super‐large mineral deposits, have been discovered. However, the genesis of manganese ore deposits is still controversial and remains a long‐standing source of debate; there are several viewpoints including biogenesis, hydrothermal sedimentation, gravity flows, cold‐spring carbonates, etc. Geochemical data from several manganese ore deposits show that there are positive correlations between Al₂O₃ and TiO₂, SiO₂, K₂O, and Na₂O, and strong negative correlations between Al₂O₃ and CaO, MgO, and MnO in black shales and manganese ores. U, Mo, and V show distinct enrichment in black shales and inconspicuous enrichment in Mn ores. Ba and Rb show strong positive correlations with K₂O in manganese ores. Cu, Ni, and Zn show clear correlations with total iron in both manganese ores and black shales. ∑REE of manganese ores has a large range with evident positive Ce anomalies and positive Eu anomalies. The Post Archean Australian Shale (PAAS) normalized rare earth element (REE) distribution patterns of manganese ores present pronounced middle rare earth element (MREE) enrichment, producing “hat‐shaped” REE plots. ∑REE of black shales is more variable compared with PAAS, and the PAAS‐normalized REE distribution patterns appear as “flat‐shaped” REE plots, lacking evident anomaly characteristics. δ¹³C values of carbonate in both manganese ores and the black shales show observable negative excursions. The comprehensive analysis suggests that the black shales formed in a reducing and quiet water column, while the manganese ores formed in oxic muddy seawater, which resulted from periodic transgressions. There was an oxidation–reduction cycle of manganese between the top water body and the bottom water body caused by the transgressions during the early Datangpo, which resulted in the dissolution of manganese. Through the exchange of the euphotic zone water and the bottom water, and episodic inflow of oxygenated water, the manganese in the bottom water was oxidized to Mn‐oxyhydroxides and rapidly buried along with algae. In the early diagenetic stage, Mn‐oxyhydroxides were reduced and dissolved in the anoxic pore water and then transformed into Mn‐carbonates by reacting with HCO₃^? from the degradation of organic matter or from seawater. In the intervals between transgressions, continuous supplies of terrigenous clastics and the high productive rates of organic matter in the euphotic zone resulted in the deposition of the black shales enriched in organic matter.     

长江中下游成矿带陆内斑岩型矿床的成岩成矿作用

陆内环境斑岩型矿床的发现对斑岩成矿理论的完善具有重要意义。长江中下游成矿带作为中国东部重要的陆内成矿带之一,成矿带内发育多个重要的斑岩型矿床,如铜山口Cu-Mo矿床、鸡冠嘴Cu-Au矿床、白云山Cu矿、城门山Cu-Mo矿床、武山Cu-Mo矿床、丰山洞Cu-Au矿床、丁家山Cu矿、洋鸡山Au矿、沙溪Cu-Au矿床、冬瓜山Cu-Au矿床、舒家店Cu矿床和安基山Cu矿床等。本文选取成矿带内典型的、具有代表性的斑岩型矿床,对其地质特征(地层、构造、含矿斑岩、脉体特征和围岩蚀变)、成岩成矿年代、成矿岩体的岩石化学和成岩成矿地球化学等方面的研究资料和成果进行了系统总结,讨论和试图阐明长江中下游成矿带陆内斑岩型矿床的成岩成矿作用与成矿模式。研究显示,长江中下游成矿带形成于燕山期陆内造山过程,成矿斑岩岩浆活动和成矿作用主要发生于149~105Ma之间,进一步可以分为早、中、晚三阶段:149~135Ma、133~125Ma和123~105Ma,三阶段岩浆活动和成矿作用主要发生于成矿带中的断隆区,早阶段(149~135Ma)和晚阶段(123~105Ma)多为斑岩-矽卡岩型矿化,中阶段(133~125Ma)矿化为典型的斑岩型矿化。长江中下游成矿带内斑岩型矿床的含矿斑岩为高钾钙碱性-钙碱性系列岩石,大部分具有埃达克岩的地球化学特征,可能为源自富集地幔的岩浆和加厚下地壳部分熔融的岩浆混合的产物,源自富集地幔的基性岩浆对成矿具有至关重要的作用,它的混入使得混合岩浆富水、硫和金属(Cu、Au)等。进一步通过与岩浆弧环境的斑岩型矿床对比研究发现,长江中下游成矿带斑岩型矿床一般不发育高级泥化岩帽(advanced argillic liithocaps)以及浅部的高-中硫矿化蚀变系统,含矿岩浆源区性质和成矿物质来源等与岩浆弧环境的斑岩型矿床明显不同。     

镇康芦子园铅锌矿床特征及成因

芦子园铅锌矿产于镇康复背斜核部寒武系沙河厂组大理岩、板岩、片岩地层中，沿背斜轴部产生的断层及层间破碎带是主要的容矿构造，成矿物质来源于地层、酸性及基性岩浆热液，矿床成因为沉积-热液改造叠生型铅锌矿床。     

地质工程专业普通地质认识实习教学的思考

文章针对地质工程专业中基础地质学的重要性和普地实习野外教学实际,提出在普地实习中融入地质工程专业知识教学内容。从岩石基本地质特征、力学问题和具体工程地质问题3个方面将基础地质学与地质工程专业知识进行融合、交叉。从而拓展学生视野,实现实习模式创新、内容改革,促进学生学习意识和自主学习的发展,提升专业思维。岩石成分与岩石力学性质、风化特征和水软化性关系密切,节理面的粗糙、起伏和充填物成分影响节理面抗剪、透水等特性,具体工程中的“滑坡”问题是典型的岩体剪切破坏问题,其形成的力学机制与剪节理相同。将上述问题两者联系起来的讲解丰富了普地实习的内容。文章认为普地实习中观察到的现象与地质工程专业课程中很多知识点紧密联系,在基础地质实习教学中融入上述地质工程的专业知识是完全可行性的,采取增加与地质工程专业结合的实践教学环节的办法,既扩大了学生知识面,初步提高学生专业素养,也为实现毕业后成为专业领域合格工程师和科研人员的培养目标迈出重要的第一步。     

Mesoscale linear streaks on Mars: environments of dust entrainment

Variable surface albedo features on Mars are likely caused by the entrainment and deposition of dust by the wind. Most discrete markings are associated with topographic forms or with regional slopes that serve to alter the effective wind shear stress on the surface. Some of the largest variable features, here termed mesoscale linear streaks, are up to 400 km in length and repeatedly occur in one of the smoothest regions of Mars: Amazonis Planitia. Their orientations and apparent season of variability as observed by Viking and Mars Orbiter cameras indicate linear streak formation by enhanced surface wind stresses during regional or local dust storms and during the initial stages of global dust storms. They provide an example of the ability of large-scale winds, without significant local enhancement, to initiate dust motion on Mars. The sizes and spacing of the linear streaks may be controlled by boundary layer rolls. The repetitive formation of these streaks, over a span of more than 11 Mars years, gives one measure of the stability of Mars’ eolian processes.