基于知识对象的土地管理空间数据库模型设计与实现

空间数据模型建立的目的是反映现实世界。当今的GIS系统的空间数据模型,主要反映地图制图领域的点、线、面对象管理与操作的几何知识。本文通过对比研究,发现土地管理空间概念的领域知识,包含几何知识。几何知识是依据几何特征属性识别的土地管理领域知识之一。将土地管理领域空间概念的领域知识对象化,建立与几何知识对象等价的对象组件,扩展对象关系型的空间数据模型,建立了[领域空间知识对象]+[GIS的点、线、面的几何对象]+[扩展属性]的空间数据模型。这种模型简化了空间数据库的管理操作,降低了对工作人员制图专业知识的要求,降低了空间对象实例与其属性的耦合度,减少了政策变化对数据的影响程度,提高了数据的稳定性和共享度。鉴于这种空间数据库模型,本文开发了空间知识对象的江苏省515城乡一体化地籍系统的数据检查子系统,在镇江市、江都市等多个市县的515城乡一体化地籍调查的数据检查入库工作中得以应用,证明了模型设计的可行性,收到了良好的效果,为专题GIS空间数据管理,提供了一种的新的空间数据模型。     

用图形演绎C程序运行的研究

说明了用图形方式展现C程序运行情况的必要性和可行性;介绍了用图形演绎C程序运行的总设计思想;详细介绍了图形界面设计要求和程序模块的功能要求。     

基于“要素对象空间信息指纹”的变化空间数据同步技术的研究

随着空间数据库的建设和应用的发展,空间数据动态更新和数据分发成为确保数据现势性的主要研究课题,系统提出将地形地物要素数据的坐标数组通过MD5算法生成32位字符串的"要素对象空间信息指纹"作为判定要素数据变化的方法,结合Oracle数据库CDC技术,快速获取空间变化数据,再通过ETL数据同步机制流程化管理空间同步过程,多节点、多级联按需配置同步图层,实现不同Oracle数据库版本、不同Arc SDE版本间的空间数据断点续传同步功能。     

一种签字工作流的定义方法研究

对签字的基本模型进行了总结，并提出一种有足够建模能力、便于用户理解与计算机实现的签字过程定义方法——带条件的链表描述法。     

导向钻机液压管路的优化设计

导向钻机液压管路的尺寸直接影响着能量损失以及管路体积、质量的大小。采用优化设计方法,综合考虑能量损失及管路体积2方面的影响,建立了导向钻机吸油管路的目标函数,经编程求解,确定了管路的合理尺寸。     

Comparison of some properties of star forming galaxies and active galactic nuclei between two BOSS galaxy samples from SDSS DR9

Using the LOWZ and CMASS samples of the ninth data release(DR9)from the SDSS-III Baryon Oscillation Spectroscopic Survey(BOSS), I investigate properties of star forming galaxies and active galactic nuclei(AGNs). The CMASS sample seriously suffers from the radial selection effect, even within the redshift0.44 ≤ z ≤ 0.6, which will likely lead to statistical conclusions in the CMASS sample being less robust. In the LOWZ sample, the fraction of star-forming galaxies is nearly constant from the least dense regime to the densest regime; the AGN fraction is also insensitive to the local environment. In addition, I note that in the LOWZ sample, the distributions of stellar mass and stellar velocity dispersion for star forming galaxies and AGNs are nearly the same.     

On an analytical framework for voids: their abundances, density profiles and local mass functions

We present a general analytical procedure for computing the number density of voids with radius above a given value within the context of gravitational formation of the large-scale structure of the Universe out of Gaussian initial conditions. To this end, we develop an accurate (under generally satisfied conditions) extension of the unconditional mass function to constrained environments, which allows us both to obtain the number density of collapsed objects of certain mass at any distance from the centre of the void, and to derive the number density of voids defined by collapsed objects. We have made detailed calculations for the spherically averaged mass density and halo number density profiles for particular voids. We also present a formal expression for the number density of voids defined by galaxies of a given type and luminosity. This expression contains the probability for a collapsed object of certain mass to host a galaxy of that type and luminosity (i.e. the conditional luminosity function) as a function of the environmental density. We propose a procedure to infer this function, which may provide useful clues as to the galaxy formation process, from the observed void densities.     

Spatial orientations of galaxies in 10 Abell clusters of BM type II–III

We present an analysis of the spatial orientations of 1315 galaxies in 10 Abell clusters of BM type II–III (type II–III in the Bautz–Morgan system). It is found that the spin-vector orientations of the galaxies in six clusters (Abell 168, 426, 1035, 1227, 1367 and 1904) tend to lie parallel to the Local Supercluster (LSC) plane. The spin-vector projections of galaxies in six clusters (Abell 168, 1020, 1035, 1227, 1904 and 1920) are found to be oriented perpendicular with respect to the direction of the LSC centre. Three clusters (Abell 1920, 2255 and 2256) show a bimodal orientation: spin vectors tend to be oriented both parallel and perpendicular to the LSC plane. No dependence of radial velocity, distance and cluster magnitude on galaxy orientation is noticed. In a comparison with previous work, we noticed that the anisotropy might increase from early-type (BM type I) to late-type (BM types II–III and III) clusters. We notice a vanishing angular momentum for the less massive galaxy clusters (richness class 0). A significant alignment of the angular momenta of galaxies for massive clusters, e.g. the core of the Shapley Supercluster (richness class 4,   M > 10¹⁵ M_⊙  ), is found.