基于二分法的多边形自动划分算法

提出一种基于面积比的多边形自动划分算法,在给定初始划分方案线的基础上研究利用二分法实现3种不同条件下多边形的自动划分,并在.NET平台下采用C#语言基于ArcGIS Engine组件进行具体实现,给出最大允许误差的取值范围。试验证明,该方法能够简化多边形自动划分的难度,提高多边形划分的自动化程度和速度,同时能保证划分结果的精确性。     

二连盆地哈达图铀矿床综合物化探特征及找矿意义

二连盆地哈达图铀矿床是我国大型可地浸砂岩型铀矿床,矿体埋深大、品位富,研究其地电化学等综合物化探特征,可为建立覆盖区航放异常有效查证技术方法提供依据.基于矿床地质及航磁航放特征的分析,开展组合物化探方法测量及特征分析.研究表明:哈达图铀矿床位于受断裂构造控制的北东向、北北东向中等磁场区及中等-弱磁场的梯度带;航空及地面...     

用红外和水汽两个通道的卫星测值指定云迹风的高度

提出了一种改进的用红外和水汽两个通道的测值指定云迹风高度的算法。利用红外水汽散点图和云迹风本身自动地将有低云的目标区、有半透明卷云的目标区、有密蔽高云的目标区分开。在有低云的目标区和有密蔽高云的目标区用红外一个通道指定云高。在有半透明卷云的目标区用红外和水汽两个通道指定云高。在用两个通道的测值指定云高时，假定卷云高度以上不存在水汽，以红外和水汽两个通道亮温相同这个方程与两个通道辐射测值线性相关的方程联立解出云的高度     

西非金矿床类型及时空分布规律

西非素有"黄金海岸"之称,近年西非金矿勘查和产量不断突破新高,已超过南非成为非洲最重要的产金区.通过系统总结西非156个有储量数据的金矿山信息发现,西非已发现金矿储量全球占比超7％,未来可能成为全球金矿开采与供应的重要一极.成因类型上以造山型金矿为主,且成矿流体具有富水含碳为特征.砾岩型金矿次之,独居特色,其他类型矿床...     

基于Google Earth的巴尔喀什湖流域中下游水资源开发利用研究

 常规的信息收集渠道难以获取国际河流研究所需的有效信息,探索新的信息收集方式对资料稀缺区开展水文水资源研究十分必要且关键。在Internet海量信息中,Google Earth（GE）平台的出现,为资源环境、交通规划等诸多领域提供了“身临其境”的远距离信息检索模式。通过基于GE平台的资料稀缺区水资源开发利用状况评价的应用框架和评价方法,并以巴尔喀什湖流域中下游为例开展了应用研究。结果表明：GE平台可成为资料稀缺区水资源开发利用研究的有效信息收集手段,文中所提出的框架、应用流程和评价方法具有较好的可操作性;研究区在1990年初就形成了以伊犁河中下游为主体、准噶尔区与巴尔喀什湖北部诸小河为重要用水区的基本格局;随着研究区经济社会发展的剧烈波动,其用水量经历了“增长-顶峰-剧减-恢复性增长”的演变格局,目前其用水量预计已恢复至20世纪80年代中期的水平,即65×108 m3左右。     

城市地表灰尘重金属研究进展及展望

城市地表灰尘是城市环境科学研究的对象之一,在对国内外有关城市灰尘概念界定研究成果进行总结的基础上,对城市地表灰尘提出新的概念和新的认识。城市地表灰尘是城市生态环境中具有环境指示作用的地表颗粒物,是含有重金属、多环芳烃等多种污染物的源与汇。对国内外地表灰尘重金属的含量水平、时空分布特征、迁移循环、赋存形态及生物有效性等方面的研究成果进行比较系统的阐述;灰尘中重金属的来源识别的方法主要有GIS空间分析,元素示踪技术,统计学方法等。并提出在今后的研究中应进一步完善城市地表灰尘中重金属的时间变化规律、地表灰尘在环境中的滞留时间、粒径的划分以及区域人体健康影响及风险评估模型优化四个方面的研究。     

Dynamic evolution model of isothermal voids and shocks

We explore self-similar hydrodynamic evolution of central voids embedded in an isothermal gas of spherical symmetry under the self-gravity. More specifically, we study voids expanding at constant radial speeds in an isothermal gas and construct all types of possible void solutions without or with shocks in surrounding envelopes. We examine properties of void boundaries and outer envelopes. Voids without shocks are all bounded by overdense shells and either inflows or outflows in the outer envelope may occur. These solutions, referred to as type void solutions, are further divided into subtypes and according to their characteristic behaviours across the sonic critical line (SCL). Void solutions with shocks in envelopes are referred to as type voids and can have both dense and quasi-smooth edges. Asymptotically, outflows, breezes, inflows, accretions and static outer envelopes may all surround such type voids. Both cases of constant and varying temperatures across isothermal shock fronts are analyzed; they are referred to as types and void shock solutions. We apply the ‘phase net matching procedure’ to construct various self-similar void solutions. We also present analysis on void generation mechanisms and describe several astrophysical applications. By including self-gravity, gas pressure and shocks, our isothermal self-similar void (ISSV) model is adaptable to various astrophysical systems such as planetary nebulae, hot bubbles and superbubbles in the interstellar medium as well as supernova remnants.      

Period investigation of two RS CVn-type binary stars: RU Cancri and AW Herculis

Orbital period variations of two RS CVn-type binaries, RU Cnc and AW Her, are presented based on the analysis of all available times of light minima. It is discovered that the orbital period of RU Cnc shows two possible period oscillations with periods of 13.38(±0.23) and 37.6(±3.4) years. The corresponding amplitudes of the oscillations are about 0.0098(±0.0023) and 0.0119(±0.0017) days. For AW Her, it is found that the period shows a cyclic variation with a period of 12.79(±0.34) years and an amplitude of about 0.0327(±0.0063) days. Since RU Cnc and AW Her are two RS CVn-type systems, the cyclic period oscillations are more likely to be caused by the magnetic activity cycles.     

The long-term multiband optical observations and colour index for the quasar 3C 273

The long baseline simultaneous multiband ( BVRI ) observations of blazar 3C 273 are presented. We have made 758 optical multiband observations with the Yunnan Astronomical Observatory (YAO) 103 cm and Shanghai Astronomical Observatory (SHAO) 156 cm from 2003 January to 2005 April. In our observational campaign, the average colour indices are   B − V = 0.21, V − R = 0.26  and   R − I = 0.31  . The mean magnitudes in B, V, R and I are 12.895, 12.698, 12.441 and 12.139, respectively. The source is in a steady state over observational campaign. The correlations between colour index and brightness are discussed. We find that the correlations of   B − V   versus B ,   V − R   versus V and   R − I   versus R have significant negative correlation, while   B − V   versus V ,   V − R   versus R and   R − I   versus I have positive correlation. These strong correlations imply that the spectrum becomes bluer (flatter) when the source becomes brighter, and redden (softer) when the source fades both in intraday and long-term variability. The spectral evolution trends of 3C 273 are consistent with those of BL Lac objects.     

Does heating by AGN shocks affect abundance profiles in galaxy clusters?

We evaluate the impact of gas shock heating by a central active galactic nuclei (AGN) in M87 on the radial distribution of heavy elements. The propagation of a shock creates an inverted entropy profile, and the subsequent rearrangement of the gaseous atmosphere transports metal-rich gas from the central region to larger radii. We show that for the parameters of the relatively weak shock, recently found in M87, the abundance profile is not strongly affected by the redistribution of the shock heated gas (except for the very central region). At the same time, the energetics of the source is fully sufficient to broaden the metal distribution to match the observations, strongly suggesting that mechanisms other than direct shock heating must operate in cluster cores. The absence of a very strong abundance peak at the very centre of M87 suggests that the central AGN produces frequent (every few 10 Myr) and relatively weak outbursts, rather than rarer (every few 100 Myr) and an order of magnitude more powerful events.