大裂隙堵漏剂在神农架矿区复杂地层钻进中的试验应用

通过大裂隙堵漏剂在神农架矿区复杂地层钻进的试验应用,论述了该堵漏剂堵漏性能参数及堵漏机理,总结了用该堵漏剂堵漏的操作方法;简述了野外施工试验的应用过程及应用效果。     

澳大利亚西部哈默斯利铁成矿省BIF富铁矿的成矿特征与控矿因素

澳大利亚西部哈默斯利铁成矿省含有世界级高品位的赤铁矿体。主要铁矿床包括芒特维尔贝克、汤姆普莱斯山、帕拉伯杜等,它们均产于元古宙早期布罗克曼BIF型含铁建造中。高品住铁矿体的空间分布明显受到元古宙区域隆起和拉张环境下形成的古老正断层系统的控制。该成矿省高品位铁矿层的形成可分为3个阶段：第1阶段为深层阶段,该阶段硅从含铁建造中淋滤出来,留下薄层状富含铁氧化物、碳酸盐岩、硅酸镁和磷灰石的残余物;第2阶段为深部大气水氧化阶段,该阶段含铁建造的磁铁矿-菱镁矿组合被氧化为赤铁矿-铁白云石,并以发育假象赤铁矿为特征;第3阶段为浅层风化作用。通过对成矿特征和成矿模式的总结,认为成矿时代、断层、褶皱等构造特征及流体和表生风化作用是富铁矿床形成的主要控矿因素。     

新疆塔里木盆地哈拉奇地区晚石炭世一早二叠世哈拉奇组的建立

哈拉奇组为新疆阿合奇县开展1：5万区域地质矿产调查工作时建立的岩石地层单位,分布在新疆阿合奇县哈拉奇地区北部,主要为一套深水碳酸盐沉积,与该区南部属碳酸盐台地沉积的康克林组在岩性、岩石组合及古生物组合上形成明显的差别。通过对该组重力流成因的生物屑砾屑灰岩中古生物化石的研究,确定其筵带为Triticites带和Pseudoschwagerina带,进而确定该组地质时代为晚石炭世-早二叠世,与南区康克林组为同时异相沉积。哈拉奇组的建立完善了该地区上石炭统一下二叠统的地层系统,确定了该地区晚石炭世-早二叠世台地边缘斜坡相的存在,对塔西北地区晚石炭世-早二叠世岩相古地理研究具有重要意义。     

贵州册亨岩架黑苗湾组的发现及其地质意义

作者在册亨尾排金矿普查地质填图工作中,于岩架镇高苕一带发现晚三叠世卡尼早期地层.根据岩性特征,将其划为黑苗湾组.本文对该地黑苗湾组的出露与分布及岩石地层特征进行详细介绍,并讨论其地质意义.     

拉萨地块西段典中组火山岩岩浆作用过程及其地质意义

拉萨地块西段分布有大面积的古近纪火山岩,蕴含着丰富的地质信息。文章对措勤地区典中组火山岩年代学、地球化学的研究表明,典中组火山岩岩浆活动在晚白垩世晚期已经开始,之后逐步向东迁移,时间上一直持续到古新世。印度板块与亚洲板块碰撞可能是从西段开始的,之后逐渐向东碰撞过渡。典中组火山岩岩浆形成的过程中发生了部分熔融作用,且在成岩过程中发生了混合作用;典中组火山岩是岛弧型俯冲向碰撞过渡过程中产生的具有岛弧或陆缘弧特点的火山岩。     

长江经济带城市水资源利用效率的空间关联网络及形成机制

探讨城市水资源利用效率空间关联网络特征及其形成机制可为实现区域用水效率协同提升提供新的政策视角。本文以长江经济带107个地级及以上城市为研究样本,首先,利用随机前沿分析法（SFA）测算出其2009—2018年水资源利用效率,并基于此构建其空间关联矩阵,继而采用社会网络分析法考察城市水资源利用效率空间关联网络的整体结构、个体结构及其空间聚类方式,最后采用二次指派程序法探讨网络形成机制。结果表明：① 城市水资源利用效率整体仍处于较低水平,但研究期内提升显著,空间关联网络格局显现,且整体网络可达性较强,几乎不存在非对称性可达的联系对,仍存在关联不紧密、网络结构稳定性欠佳等问题;② 上中下游地区的中心城市发挥着中心行动者、中介沟通者的重要作用,呈现“中心城市—非中心城市”的“核心—边缘”空间分布特征;③ 城市水资源利用效率空间关联板块可划分为净溢出、主受益和双向溢出板块,各板块成员组成符合长三角城市群、长江中游城市群、成渝城市群的分布特征;④ 城市间地理邻近性差异、经济发展水平差异、对外开放程度差异等自然地理条件和社会经济因素对城市水资源利用效率关联网络的形成具有显著影响。     

The Zeeman effect in the Sobolev approximation: applications to spherical stellar winds

Modern spectropolarimeters are capable of detecting subkilogauss field strengths using the Zeeman effect in line profiles from the static photosphere, but supersonic Doppler broadening makes it more difficult to detect the Zeeman effect in the wind lines of hot stars. Nevertheless, the recent advances in observational capability motivate an assessment of the potential for detecting the magnetic fields threading such winds. We incorporate the weak-field longitudinal Zeeman effect in the Sobolev approximation to yield integral expressions for the flux of circularly polarized emission. To illustrate the results, two specific wind flows are considered: (i) spherical constant expansion with   v ( r ) = v _∞  and (ii) homologous expansion with   v ( r ) ∝ r   . Axial and split monopole magnetic fields are used to schematically illustrate the polarized profiles. For constant expansion, optically thin lines yield the well-known 'flat-topped' total intensity emission profiles and an antisymmetric circularly polarized profile. For homologous expansion, we include occultation and wind absorption to provide a more realistic observational comparison. Occultation severely reduces the circularly polarized flux in the redshifted component, and in the blueshifted component, the polarization is reduced by partially offsetting emission and absorption contributions. We find that for a surface field of approximately 100 G, the largest polarizations result for thin but strong recombination emission lines. Peak polarizations are approximately 0.05 per cent, which presents a substantial although not inconceivable sensitivity challenge for modern instrumentation.     

Evolution of the mass function of dark matter haloes

We use a high-resolution ΛCDM numerical simulation to calculate the mass function of dark matter haloes down to the scale of dwarf galaxies, back to a redshift of 15, in a  50 h ⁻¹ Mpc  volume containing 80 million particles. Our low-redshift results allow us to probe low-σ density fluctuations significantly beyond the range of previous cosmological simulations. The Sheth & Tormen mass function provides an excellent match to all of our data except for redshifts of 10 and higher, where it overpredicts halo numbers increasingly with redshift, reaching roughly 50 per cent for the  10¹⁰–10¹¹ M_⊙  haloes sampled at redshift 15. Our results confirm previous findings that the simulated halo mass function can be described solely by the variance of the mass distribution, and thus has no explicit redshift dependence. We provide an empirical fit to our data that corrects for the overprediction of extremely rare objects by the Sheth & Tormen mass function. This overprediction has implications for studies that use the number densities of similarly rare objects as cosmological probes. For example, the number density of high-redshift  ( z ≃ 6) QSOs  , which are thought to be hosted by haloes at 5σ peaks in the fluctuation field, are likely to be overpredicted by at least a factor of 50 per cent. We test the sensitivity of our results to force accuracy, starting redshift and halo-finding algorithm.