基于EOS-MODIS的广西全境石漠化信息提取方法研究

喀斯特石漠化是发生在亚热带岩溶地貌中的土地退化过程,其显著特征为土壤严重侵蚀、基岩裸露、植被退化、土地生产力下降。石漠化既制约当地的经济发展,又可能引起小环境气候的恶化,同时也破坏生物多样性,危及生态环境自然景观。因此,研究石漠化,分析其成因和分布特征对喀斯特地区的防灾减灾以及可持续发展具有十分重大的意义。EOS-MODIS数据所固有的优点(获取便捷、覆盖范围广、成像周期短),使其成为理想的大范围石漠化研究的潜在遥感数据源。     

黄骅坳陷北大港构造带沙河街组沉积体系定量研究

针对陆相湖盆沉积特征,以T A Cross高分辨率层序地层学理论为指导,在大量岩心、测井和地震资料研究的基础上,定量研究了黄骅坳陷北大港构造带沙河街组沉积体系和沉积物源特征,确定了沙河街组沉积时期总体发育近岸水下扇、滩坝、深水重力流水道、扇三角洲前缘和滑塌浊积扇等主要沉积相类型。中期基准面旋回A-D层序沉积时期发育近岸水下扇和扇三角洲前缘—前扇三角洲—滑塌浊积扇沉积体系;中期基准面旋回E-F层序沉积期间发育有利于油气储集的近岸水下扇和滩坝砂体;中期基准面旋回G层序沉积时期主要发育重力流主水道—重力流水道侧缘以及近岸水下扇沉积砂体;中期基准面旋回H层序沉积时期主要发育重力流主水道—重力流水道侧缘沉积体系。最后,预测了有利岩性圈闭发育的沉积相带和地区。     

塔里木盆地塔中低凸起地层水化学特征对不整合的响应

对塔中低凸起地层水化学特征与不整合之间关系的研究结果表明,地层水化学特征对不整合具有很好的响应。在遭受强烈抬升和剥蚀、之间形成不整合的奥陶系和志留系,以及紧靠不整合面附近的石炭系CⅢ油组,其地层水具有矿化度、Cl-含量、K Na 含量和r(Cl-Na)/rMg值相对较小,而HCO3-含量、rNa/rCl值和rSO42-×100/rCl值相对较大的特点,反映出地质历史时期大气降水的影响。在志留系与石炭系之间以及志留系与奥陶系之间的不整合面附近,地层水的矿化度、r(Cl-Na)/rMg值和B3 含量变小,而rNa/rCl值和rSO24-×100/rCl值变大,具有典型的遭受大气淋滤的地层水化学基本特征。     

黄骅坳陷埕北断坡不整合特征与油气成藏

黄骅坳陷埕北断坡处于歧口凹陷向埕宁隆起过渡的斜坡带上,发育多个不整合,这些不整合对该区的油气成藏起重要作用。利用地震资料,在剖面上将不整合划分为5种类型：褶皱不整合、断褶不整合、削截不整合、超覆不整合、平行不整合。其中平行不整合分布在凹陷区,褶皱不整合分布在基底,断褶不整合分布在大断裂下降盘,削截不整合分布在大断裂上升盘,而超覆不整合多分布在隆起斜坡区;利用测井资料,在纵向上将不整合划分为3层结构：不整合面之上岩石、风化粘土层及半风化岩石,由于每层结构的岩性与厚度不同,形成ACE型、ADE型、BCE型和BDF型4种岩性配置模式。不整合构成埕北断坡油气侧向运移的重要通道,同时在其之上形成超覆不整合油气藏,在其之下依靠风化粘土层遮挡形成削截不整合与褶皱不整合油气藏。勘探证实,研究区众多油气显示或油气藏均位于不整合面上、下50 m范围内。开展不整合与油气成藏关系研究,将拓宽黄骅坳陷隐蔽油气藏的勘探空间,对我国东部油气资源挖潜具有重要的理论与实践意义。     

单侯井田构造发育规律及其对煤层开采的影响

从区域构造入手,对单侯井田构造进行分析,认为井田内断层发育以走向NW—NE、落差≤5m的小型正断层为主,且主要分布于大中型构造的两侧．特别是在其弧形转折带附近往往形成“羽”状雁列的小断层密集带。断层垂向上多分布于4—7号煤层之间的厚煤层发育区,其严重破坏了煤层的连续及完整性,是影响煤层开采的最主要因素之一。井田褶皱构造相对不发育,以短轴小型背、向斜为主,均属缓波状褶曲,对煤层的开采无影响或影响较小。根据井田地质构造发育程度,对其进行预测及分区评价：井田东部为强烈的构造挤压带,以发育走向NW-近EW—NE向的大型逆掩断层为特点,构造最复杂;井田西北部是相对较轻微的构造挤压带,以发育走向NE向的逆断层为特征,构造较复杂;井田南部以发育近SN或NNW向正断层为主,构造相对简单。评价结果对矿井设计及采区与工作面布置有一定的指导作用。     

地震勘探测量数据的快速处理和管理

目前山区地震测量施工主要的困难体现在山区放样难、内业数据处理复杂、测量成果无法进行异常检查等方面,其严重影响后续资料处理和解释质量。针对以上难点,利用AUTOCAD为平台,开发了一套物探测量数据处理系统。该系统具有展点、点内插、绘制测线剖面图、管理测点信息、打印成果报表等功能,实现了地震勘探测量数据的快速处理及有效检核．提高了野外测量放样的施工效率和数据的准确度。另外其图层管理及系统辅助功能,还可为地震勘探施工设计提供参考。     

应用全站仪进行三角高程测量方法的探讨

传统的三角高程水准测量由于受地形起伏的限制,外业工作量大,施测精度和工作效率不高。本文采用全站仪对传统的三角高程水准测量方法进行了改进,并论述了全站仪三角高程测量方法的原理和实际作业方法。     

震灾保险研究中的软科学问题

震灾保险研究融会着自然科学与社会科学的紧密结合和相互渗透,基于这一认识,本文联系震灾保险的社会属性,分析并指出这一险种的非强制性质;保护应用的权益与责任;对社会不规范投保行为的制约;正确理解“与国际惯例接轨”、地震系统的协作模式、政府部门的政策导向等等带有根本性的问题,以启示人们把握研究的大方向,从而加快我国该项研究的实用化进程。     

Spatial orientation of the spin vectors of the disk galaxies in the Virgo cluster I. A catalogue of the disk galaxies in the Virgo cluster

Based on four UK Schmidt Telescope (UKST) IIIa-j direct plates which had been digitized by the Automated Plate Measuring System (APM), a detailed identification of the disk galaxies in the Virgo cluster has been carried out. The certain and possible member galaxies are mainly selected from the updated Catalogue of 2096 Galaxies in the Virgo Cluster Area (VCC). The area of this identification covers a 85 square degree region centered on this cluster. As a result, we compiled a new catalogue of 340 certain and possible member disk galaxies, including 85 lenticulars (SO), 136 spirals (S) and 119 irregulars (Irr), where the APM-measured values of the position angle (P.A.) and diameters of 299 disk galaxies are provided. For at least 149 galaxies, the values of the P.A. and diameters are published for the first time.Comparison between the APM-measured P.A. and diameters of galaxies and those given by the Uppsala General Catalog of Galaxies (UGC) demonstrates the reliability of our data. The statistical properties and completeness of this database are also discussed. Compared with the UGC-given P.A. and diameters which were determined by eyes, our data has no selection effect owing to the instrument measurements. Within our searching region, this might be the largest and relatively complete photometric database published so far for investigating the spatial orientation of the spin vectors of galaxies in the Virgo cluster.     

Propagation of MHD body and surface waves in magnetically structured regions of the solar atmosphere

The fact that magnetically structured regions exist in the solar atmosphere has been known for a number of years. It has been suggested that different kinds of magnetohydrodynamic (MHD) waves can be efficiently damped in these regions and that the dissipated wave energy may be responsible for the observed enhancement in radiative losses. From a theoretical point of view, an important task would be to investigate the propagation and dissipation of MHD waves in these highly structured regions of the solar atmosphere. In this paper, we study the behavior of MHD body and surface waves in a medium with either a single or double (slab) magnetic interface by use of a nonlinear, two-dimensional, time-dependent, ideal MHD numerical model constructed on the basis of a Lagrangean grid and semi-implicit scheme. The processes of wave confinement and wave energy leakage are discussed in detail. It is shown that the obtained results depend strongly on the type of perturbations imposed on the interface or slab and on the plasma parameter, . The relevance of the obtained results to the heating problem of the upper parts of the solar atmosphere is also discussed.