水库大坝表面变形观测的方法探讨     

郭重辉 《现代测绘》2007,30(2):17-18

本文主要阐述了风城水库大坝表面变形观测各种工作点的布设、大坝变形观测的方法及效果、大坝变形的数据分析过程等,旨在与同行们共同交流探讨变形观测的方法.  相似文献   

武汉台形变观测与降雨参数之间的定量分析与研究          下载免费PDF全文

吕琳  杨艳芳  舒德亮 《地震工程学报》2020,42(1):136-142

基于“前兆台网(站)观测数据跟踪分析平台”,对武汉台形变观测资料进行了系统分析,提取出观测曲线受降雨干扰影响的事件,采用降雨总量、初始驱动降雨量和瞬时降雨量最大值等降雨参数对降雨干扰事件进行统计分析。结果表明:降雨总量达40 mm、初始驱动降雨量为0.3 mm或瞬时降雨量最大值达0.6 mm时,DSQ型水管倾斜仪易受降雨干扰;SSY型铟瓦棒伸缩仪当降雨总量超60 mm或瞬时降雨量最大值大于0.5 mm时易受降雨干扰;VS型垂直摆倾斜仪受降雨干扰与降雨总量、初始驱动降雨量和瞬时降雨量最大值无显著相关关系;降雨总量对形变仪器观测物理量的影响基本呈现线性;而形变仪器观测物理量与初始驱动降雨量、瞬时降雨量最大值无显著相关关系。认为武汉台形变观测受降雨影响主要来自降雨渗透影响和周边水体荷载变化影响两个方面。  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   

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

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Stellar models for very low-mass main-sequence stars: the role of model atmospheres     

Brocato  Cassisi  & Castellani 《Monthly notices of the Royal Astronomical Society》1998,295(3):711-724

We present very low-mass stellar models as computed using non-grey model atmospheres for selected assumptions about the stellar metallicities. The role of atmospheres is discussed and the models are compared with models based on the Eddington approximation, and with similar models that have appeared in the recent literature. Theoretical predictions concerning both the HR diagram location and the mass–luminosity relation are presented and discussed in terms of expectations in selected photometric bands. Comparison with available observational data concerning both galactic globular clusters and dwarfs in the solar neighbourhood reveals a satisfactory agreement together with the existence of some residual mismatches.  相似文献   

Mass segregation in young stellar clusters     

Ian A. Bonnell  & Melvyn B. Davies 《Monthly notices of the Royal Astronomical Society》1998,295(3):691-698

We investigate the evolutionary effect of dynamical mass segregation in young stellar clusters. Dynamical mass segregation acts on a time-scale of order the relaxation time of a cluster. Although some degree of mass segregation occurs earlier, the position of massive stars in rich young clusters generally reflects the cluster's initial conditions. In particular, the positions of the massive stars in the Trapezium cluster in Orion cannot be due to dynamical mass segregation, but indicate that they formed in, or near, the centre of the cluster. Implications of this for cluster formation and for the formation of high-mass stars are discussed.  相似文献   

Spectroscopic observations of the eclipsing polar MN Hya (RX J0929–24)     

Gavin Ramsay  & Peter J. Wheatley 《Monthly notices of the Royal Astronomical Society》1998,301(1):95-100

We present low–medium resolution optical spectroscopy of the eclipsing AM Her system MN Hya (RX J0929–24). We determine the magnetic field strength at the primary accretion region of the white dwarf to be 42 MG from the spacing of cyclotron features visible during π ∼ 0.4–0.7. From spectra taken during the eclipse we find that the secondary has an M3–4 spectral type. Combined with the eclipse photometry of Sekiguchi, Nakada &38; Bassett and an estimate of the interstellar extinction we find a distance of ∼300–700 pc. We find unusual line variations at π ∼ 0.9: Hα is seen in absorption and emission. This is at the same point in the orbital phase at which a prominent absorption dip is seen in soft X-rays.  相似文献