苏通大桥钢箱梁制造几何控制三维高精度基准网测设     

张云青  徐良 《现代测绘》2007,30(5):19-21

本文详细介绍了对苏通大桥主桥钢箱梁制造几何控制三维高精度基准网的测设，通过实际工程的实施对高精度三维基准网的方案设计和精度控制进行了有效的探索。  相似文献   

省级基础地理信息数据更新方法探讨     

姜建慧 《东北测绘》2007,30(6):89-91

主要从更新方法、技术方案及数据共享方面讨论了省级基础地理信息数据更新的相关问题。  相似文献   

对地观测卫星地面站的站址选择和布局分析     

胡国军  李世忠胡燕 杨喆 《测绘科学与工程》2007,27(3):22-26

现代小卫星技术是近些年来迅速发展起来的航天领域高新技术，利用该技术为地球观测服务是一件远景可观、意义深远的事情。在对地观测卫星的诸多关键技术之中，地面站的设计是一个很重要的方面。本文主要对对地观测卫星地面站的站址选择与布局进行了详细的讨论。  相似文献   

北美五大湖水环境保护经验分析     

窦明  马军霞  胡彩虹 《河南气象》2007,(2)

介绍了位于美国和加拿大边界的世界上最大的淡水水体——北美五大湖的基本情况及水环境污染和治理历程,讨论美加两国政府在水环境保护方面合作的经验,概括了五大湖环境保护工作所取得的成就。实践证明,五大湖水资源综合管理体制、水环境保护策略是行之有效的。经过几十年的努力,五大湖的水质状况已有明显改善,尤其是在人群健康保障、富营养化治理和有毒物质消减方面取得了长足的进步。  相似文献   

胶西北金成矿区He、Ar同位素组成及成矿流体来源研究     

王金辉 《岩石矿物学杂志》2020,39(2):172-182

胶东半岛西北地区是我国重要的金成矿区,主要受三山岛断裂、焦家断裂、招平断裂带控制。为探讨3条主要成矿带成矿流体的来源与区别,对成矿带内典型矿床载金黄铁矿中流体包裹体进行了He、Ar同位素测试。结合前人数据表明三山岛成矿带3He/4He均值为1.95 Ra,焦家成矿带^3He/^4He均值为1.74 Ra,招平成矿带^3He/^4He均值为1.54 Ra,从西往东逐渐降低,说明地幔流体参与成矿自西往东逐渐降低。黄铁矿流体包裹体中放射性成因Ar所占比例范围三山岛成矿带1.17%~87.12%,平均33.04%,焦家成矿带15.57%~90.00%,平均55.75%,招平成矿带7.94%~92.69%,平均44.23%,说明在成矿过程中,地壳成矿流体参与成矿作用焦家成矿带最高,招平成矿带次之,三山岛成矿带最低。结合H、O稳定同位素研究,认为成矿流体主要来源于地壳,并有地幔流体加入,具地壳流体和地幔流体混合特征,上升过程中可能还有少量大气降水的参与。  相似文献   

武乡区块山西组泥页岩孔隙结构及分形特征研究     

曹磊  郭英海 《岩石矿物学杂志》2020,39(3):283-290

沁水盆地东部煤系伴生泥页岩广泛发育,页岩气资源潜力大,开展该区泥页岩孔隙结构特征的研究对页岩含气性评价及实现煤层气、页岩气合探共采具有重要意义。本文以盆地内武乡区块Y井二叠系山西组泥页岩为研究对象,通过XRD、高压压汞和低温液氮吸附等实验手段对泥页岩孔隙结构特征及分形特征进行了研究。结果表明,Y井山西组泥页岩的矿物组成以黏土矿物和石英为主;泥页岩中小于50 nm的孔隙大量发育,结构形态上以狭缝平板型孔隙和"细瓶颈"孔隙为主;泥页岩样品吸附曲线呈倒S型,属于Brunauer分类方案中的Ⅱ型曲线,其脱附曲线属于IUPAC分类方案中的H2型(兼具H1型及H3型),属De Boer分类方案中的B型(兼具E型及C型); Y井山西组泥页岩分形维数接近3,非均质性较强,矿物成分、总孔体积、平均孔径和TOC含量是影响泥页岩分形维数的重要因素。  相似文献   

High-velocity stars from decay of small stellar systems     

L. G. Kiseleva    J. Colin    B. Dauphole  & P. Eggleton 《Monthly notices of the Royal Astronomical Society》1998,301(3):759-766

In this paper we present numerical results on the decay of small stellar systems under different initial conditions (multiplicity 3 ≤  N  ≤ 10, and various mass spectra, initial velocities and initial configurations). The numerical treatment uses the CHAIN1 code (Mikkola &38; Aarseth). Particular attention is paid to the distribution of high-velocity escapers: we define these as stars with velocity above 30 km s⁻¹. These numerical experiments confirm that small N -body systems are dynamically unstable and produce cascades of escapers in the process of their decay. It is shown that the fraction of stars that escape from small dense stellar systems with an escape velocity greater than 30 km s⁻¹ is ∼1 per cent for all systems treated here. This relatively small fraction must be considered in relation to the rate of star formation in the Galaxy in small groups: this could explain some moderately high-velocity stars observed in the Galactic disc and possibly some young stars with relatively high metallicity in the thick disc.  相似文献   

Stream overflow and dwarf nova eruptions     

M. R. Schreiber  & F. V. Hessman 《Monthly notices of the Royal Astronomical Society》1998,301(3):626-630

We consider the effects of accretion stream overflow on the viscous dynamics of accretion discs in dwarf novae. If the stream from the secondary star is geometrically thick enough, some fraction of its material can flow over and under the disc. The mass and specific angular momentum of the stream are then deposited not only at the point of collision with the outer disc, but also at those radii in the inner disc with geometric heights that are large enough to intercept the residual stream, or near the radius where the disc has the same specific angular momentum as the stream. The overflowing stream can alter the behaviour of heating fronts and cooling fronts in the disc. If the mass fraction of the overflowing stream is of order tens of per cent, the deposition of mass in the inner parts of the disc is sufficient to change the character of the eruption light curves significantly.  相似文献   

The destructive effects of binary encounters on red giants in the Galactic Centre     

Melvyn B. Davies  Richard Blackwell  Vernon C. Bailey  & Steinn Sigurdsson 《Monthly notices of the Royal Astronomical Society》1998,301(3):745-753

We consider the destructive effects of encounters between binaries and red giant stars in the Galactic Centre. Such encounters may explain the observed depletion of luminous red giants within the central 0.2 pc of the galaxy. We consider encounters involving 2- and 8-M⊙ red giants, and thus span the range of stellar masses contributing to the most luminous red giants observed in the Galactic Centre. To explore the phase space of encounters thoroughly, we simulate 18 × 10³ encounters using a modified four-body code in which the red giant core and components of the binary are treated as point masses, and where the envelope configuration is assumed to remain static throughout the encounter. We then rerun a small number of encounters with a smoothed particle hydrodynamics (SPH) code to confirm the reliability of conclusions drawn from the four-body runs. We see two possible pathways to red giant destruction. A large fraction of encounters lead to the formation of common-envelope systems, where two compact objects (drawn from the red giant core and the components of the original binary) form a binary within a common gaseous envelope, whilst the third body is ejected. The destruction of the red giant will then follow when the envelope is ejected as the binary hardens. In a smaller number of encounters, the intruding binary passes through the star and ejects the red giant core from the envelope. The red giant envelope will then disperse on short time-scales. We compute the time-scales for both of these processes to occur in the Galactic Centre for a variety of binary populations.  相似文献   

The tilt of the Fundamental Plane of early-type galaxies: wavelength dependence     

M. Scodeggio    G. Gavazzi    E. Belsole    D. Pierini  & A. Boselli 《Monthly notices of the Royal Astronomical Society》1998,301(4):1001-1018

  相似文献