江西会昌岽背玄武岩地球化学和Sr-Nd同位素特征及其地质意义

江西会昌岽背地区晚中生代玄武岩的SiO2含量为49.06%～50.14%,K2O含量为1.26%～1.63%.其微量元素显示出大离子亲石元素富集,高场强元素亏损,尤以明显的Nb、Ta亏损为特征;REE总量为(135.5～146.8)×10-6,(La/Yb)N≈10,表现出LREE富集的稀土元素配分模式,且无明显的Eu异常;Sr-Nd同位素具有高(87Sr/86Sr)i(0.70678～0.70695)和低εNd(t)(-2.46～-2.18)的特征.据以上特征并结合区域地质背景,反映出岽背玄武岩的源区可能为EMⅡ型富集型大陆岩石圈地幔,其形成的构造环境为活动大陆边缘.较低的Nb/U比值(7～8)暗示该玄武质岩浆在形成过程中遭受了一定程度的大陆地壳混染或与俯冲过程有关的物质的加入.岽背玄武岩具有陆缘弧型地球化学特征,指示会昌地区在晚白垩世晚期(约85 Ma)处于活动大陆边缘的构造环境,该玄武岩的形成可能与燕山晚期古太平洋板块向欧亚大陆的俯冲消减作用关系密切.底侵作用可能为会昌地区燕山晚期成矿岩浆的生成提供了流体和热,有利于铜多金属矿的形成.     

地震条件下挡土墙主动土压力及其分布的统一解

在非地震主动土压力公式的基础上,用微分薄层法给出了地震条件下主动土压力公式,其中填土面倾斜、墙背倾斜、填土为黏性土、墙背与填土间同时存在凝聚力c和内摩擦角? 作用、墙后破裂体存在水平向和竖向的地震加速度,目前所见的地震情况下和非地震情况下的主动土压力均是此公式的特例。对上述同一条件下的挡墙用过墙踵的整块破裂体作静力平衡分析（如库仑分析）,得到的总土压力与文中微分薄层法得到的总土压力大小相等,但微分薄层法作用点位置明显增加,研究表明：设计抗震和非抗震各类挡墙时要引起足够的重视。     

城市活动断层探测中的浅层地震勘探数据库建设——以石嘴山市活动断层探测为例

浅层人工地震勘探是城市活断层探测工程中的重要部分。浅层地震勘探数据库记录测点位置、测线分布图、断点位置等详细信息。本文以宁夏石嘴山市活动断层探测为例,重点介绍了针对石嘴山市内四条隐伏断裂所布设的33条浅层地震勘探测线数据库建设的数据库模型、技术方法、操作技巧及注意事项,为城市活断层探测中基于 ArcGIS等平台系统建立浅层地震勘探数据库提供借鉴。     

中国老龄事业发展水平时空演化及其与经济发展水平的空间匹配

基于“积极老龄化”理论框架,从健康、参与和保障三大维度构建中国老龄事业发展水平评价指标体系。以中国大陆31个省（自治区、直辖市）为研究对象,运用数理统计、重心和空间重叠性、空间错位分析和计量经济模型等方法,分析了2004—2016年中国老龄事业发展水平的时序变化、空间格局、错位特征及其影响机制。结果表明：① 2004—2016年,中国老龄事业发展水平整体快速增长,区域差异逐渐缩小,但区域失衡特征不容忽视。东部地区整体水平高于中部、西部及东北地区,并伴有“西部崛起,中部及东北地区塌陷”特征。东部地区呈现“两极化”现象。② 中国老龄事业基本处于低水平发展阶段,空间分布由西南-东北辐射递减模式转变为显著的“中部塌陷”式,形成一条由北向南的低值集聚带,纵贯中国中部,与区域经济发展存在错位关系。③ 负向错位区主要分布在黄河、长江中上游地区,正向错位区主要集中在东部沿海、长城以北等地区。空间错位强度存在显著的地域差异性,其中西部地区尤为显著。④ 老龄事业发展水平的动态变化是多因素交互作用的结果。经济发展水平、政府政策和行政导向及产业结构的时空分异对其产生正向影响。市场经济规模扩大和人口老龄化未对老龄事业发展起推动作用,与理论预期不符。家庭规模小型化的倒逼作用不显著。     

我国含油气盆地的类型、构造演化和油气分布

本文以板块构造学说为基础详细讨论了我国主要含油气盆地的类型、构造演化、改造作用形成的构造和油气分布。论文指出我国含油气盆地多属板内断陷（或坳陷）叠合式盆地;油气分布主要受盆地类型、构造演化和改造作用形成的构造样式等多种因素的控制。     

Interpretation of Solar Magnetic Field Strength Observations

This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe?i to the line of Fe?i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ ^?1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ ^?1=4.15?2.82sin?²(ρ). Previously δ ^?1=4.5?2.5sin?²(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys. 213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter.     

A Chandra detection of the radio hotspot of 3C 123

Chandra X-ray Observatory observations of the powerful, peculiar radio galaxy 3C 123 have resulted in an X-ray detection of the bright eastern hotspot, with a 1-keV flux density of ∼5 nJy. The X-ray flux and spectrum of the hotspot are consistent with the X-rays being inverse-Compton scattering of radio synchrotron photons by the population of electrons responsible for the radio emission ('synchrotron self-Compton emission') if the magnetic fields in the hotspot are close to their equipartition values. 3C 123 is thus the third radio galaxy to show X-ray emission from a hotspot which is consistent with being in equipartition. Chandra also detects emission from a moderately rich cluster surrounding 3C 123, with L _X(2–10 keV)=2×10⁴⁴ erg s⁻¹ and kT ∼5 keV, and absorbed emission from the active nucleus, with an inferred intrinsic column density of 1.7×10²² cm⁻² and an intrinsic 2–10 keV luminosity of 10⁴⁴ erg s⁻¹.     

The timing of salt structure growth in the Southern Permian Basin (Central Europe) and implications for basin dynamics

In this paper, a literature‐based compilation of the timing and history of salt tectonics in the Southern Permian Basin (Central Europe) is presented. The tectono‐stratigraphic evolution of the Southern Permian Basin is influenced by salt movement and the structural development of various types of salt structures. The compilation presented here was used to characterize the following syndepositional growth stages of the salt structures: (a) “phase of initiation”; (b) phase of fastest growth (“main activity”); and (c) phase of burial’. We have also mapped the spatial pattern of potential mechanisms that triggered the initiation of salt structures over the area studied and summarized them for distinct regions (sub‐basins, platforms, etc.). The data base compiled and the set of maps produced from it provide a detailed overview of the spatial and temporal distribution of salt tectonic activity enabling the correlation of tectonic phases between specific regions of the entire Southern Permian Basin. Accordingly, salt movements were initiated in deeply subsided graben structures and fault zones during the Early and Middle Triassic. In these areas, salt structures reached their phase of main activity already during the Late Triassic or the Jurassic and were mostly buried during the Early Cretaceous. Salt structures in less subsided sub‐basins and platform regions of the Southern Permian Basin mostly started to grow during the Late Triassic. The subsequent phase of main activity of these salt structures took place from the Late Cretaceous to the Cenozoic. The analysis of the trigger mechanisms revealed that most salt structures were initiated by large‐offset normal faults in the sub‐salt basement in the large graben structures and minor normal faulting associated with thin‐skinned extension in the less subsided basin parts.     

晚型星HR5553,εEri和70 Oph的活动性,金属丰度和磁场的测定

对１９９５年１１月和１９９６年３、４月间观测获得的ＨＲ５５５３、７０Ｏｐｈ和εＥｒｉ给出了高分辨率,高信噪比的阶梯光栅光谱资料。确定了这３颗晚型活动星的大气参数,采用谱线细致分析方法求出了铁、锂、钙、钪、钛、钒、铬、锰、钴、镍、钇、锆和钡１３种金属元素的丰度。采用多重线统计方法测定了这３颗晚型活动星的磁场和磁场覆盖因子。     

TTG岩套的成因及其形成环境

TTG岩套是一类包含了三种岩性的岩石组合,即英云闪长岩(tonalite)—奥长花岗岩(trondhjemite)—花岗闪长岩(granodiorite)。TTG岩套的规模在太古宙最大,是早期陆壳的主体且在各地质历史时期均有发育。该岩石组合是岩石学定名,多数样品的地球化学特征相似:富Na,高Al2O3(平均15%),低Mg、Ni、Cr,富集LREE、亏损HREE、高Sr、低Y、低Yb且无明显的负Eu异常。其微量元素特征与Adakite(高锶低钇中酸性岩,"埃达克岩")类似。目前多数学者认同其为变玄武质岩石部分熔融后的熔体,主要争论在于其源岩的变质程度。笔者认为TTG岩套的源区不应局限于某个变质相,而是涵盖了较大的P—T范围。对于其形成环境的探讨,笔者认为应该以地球演化不同时期的地球动力学背景为前提,盲目地"将今论古"是不合理的。本文在总结前人研究成果的基础上提出3.8Ga之前的TTG岩套可能是在板块构造未启动的非俯冲条件下形成的;3.8~1.9Ga的TTG岩套产生在发育俯冲式板块构造且板块构造具有间歇式特点的背景下,此时可能既存在非俯冲环境下产出的TTG岩套也存在俯冲环境下产出的TTG岩套,而且其产出应该具有幕式特征;古元古代之后的TTG岩套可能无一例外均是俯冲板片熔融的产物。