雷暴云电结构与闪电关系初探   总被引：1，自引：13，他引：1       下载免费PDF全文

罗霞  陈渭民  李照荣  胡胜娟  李旭 《气象科学》2007,27(3):280-286

利用雷暴云偶极性电结构理论,结合卫星和雷达资料分析了不同荷电结构下地面电场。结果表明:当正电荷中心高度越高、负电荷中心高度越低,形成的地面负电场越大,越有利于地闪的形成;负地闪发生后或云砧下方,地面电场成正极性,易引发正地闪;地闪分布与雷达回波、卫星云图中雷暴云位置基本一致,结合雷达和卫星资料可初步判断正/负地闪发生位置。  相似文献   

基于规则格网数据断面极值法的一种改进方法     

刘梅余  鲍峰  欧建良 《现代测绘》2007,30(3):11-12

在研究基于规则格网数据地形特征提取过程中,主要有断面极值法和流水模拟法.在断面极值法中,针对传统断面极值法生成的特征线存在零碎、并行交叉等缺点,我们改进了传统的局部断面极值法,在特征线连接过程中增加了“将特征点邻域内其它候选特征点设置为已被引用、根据特征线长度与范围阈值筛选特征线“等条件,以克服生成的特征线存在的零碎和并行交叉问题.  相似文献   

Experimental study on the effects of artificial bed roughness on turbidity currents over abrupt bed slope change     

《国际泥沙研究》2020,35(3):256-268

A series of experimental observations are presented in the current study to discuss the effects of artificial bed roughness on the turbidity current flowing in a rectangular channel with an abrupt change in bed slope.For this purpose,two different types of elements,sinusoidal and trapezoidal,with various heights and arrangements are considered as artificial bed roughness.A Vectrino velocity meter was used to measure the velocity and sediment concentration profiles.The effects of inlet sediment concentration on front velocity,body velocity,unit discharge,sediment concentration,and suspended load transport rate also were investigated.Accurate equations were developed for estimation of the velocity of a turbidity current over smooth and rough beds.The unexpected experimental results showed that unlike the effect of roughness height,a change in the roughness arrangement has no significant influence on the velocity of a turbidity current.Also,the effect of bed roughness on the front velocity of a denser current is more significant.  相似文献   

地面-坑道激电测深方法在山东玲珑断裂带深部找矿中的应用     

李忠平 《地质与勘探》2020,56(4):783-791

在山东玲珑断裂带深部找矿中,考虑断裂带处在地电干扰和地形变化复杂地段,且深部地质体产状变化较大,仅依据半空间地面物探方法很难摸清地质体的展布形态,盲目布设钻孔会造成找矿成本的提高。为精确反演深部矿体的边界范围、走向及倾向,提高钻孔见矿率,降低找矿成本,在山东玲珑断裂带地面、坑道采用立体物探技术,试验通过布设多条方位不同的地-坑、坑-坑和地-地纵横激电中梯剖面和双向三极测深剖面,进行了二维电法剖面反演。在地面-坑道激电测深方法中,地面-坑道供电,坑道测量探测深度与坑道深度呈正相关,反映了深部巷道底板以下电阻率和极化率的分布状况,可以实现深地探测目的。由于地面-坑道供电,坑道测量装置处在半空间和全空间两个部分,需要采用"镜像法"和地下倾斜偶极源电流场特征对其装置系数k值重新推导,以反映坑道空间岩矿体真实电阻率的变化。坑道中梯剖面异常与单向三极剖面异常、双向三极电测深反演结果对应较好。经钻探验证,矿体分布与物探推断高极化体基本一致,为快速准确布设深部钻孔提供资料。  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   

A Low-Sidelobe, High Frequency Corrugated Feed Horn for CMB Observations     

M. Bersanelli  E. Mattaini  E. Santambrogio  A. Simonetto  S. Cirant  F. Gandini  C. Sozzi  N. Mandolesi  F. Villa 《Experimental Astronomy》1998,8(3):231-238

We have produced a prototype broadband, low-sidelobe conical corrugated feed horn suitable for measurements of the Cosmic Microwave Blackground (CMB) radiation in the frequency band 120–150 GHz. The antenna is a first prototype for the Low Frequency Instrument array in ESA's PLANCK mission, a space project dedicated to CMB anisotropy mesurements in the 30–900 GHz range. We describe the fabrication method, based on silver electro-formation, and present the two-dimensional antenna beam pattern measured at 140 GHz with a milimeter-wave automated scalar test range. The beam has good symmetry in the E and H planes with a far sidelobe level approaching –60 dB at angles 80°. An upper limit to the return loss was measured to be –21 dB.  相似文献   

精密时钟单钟幂律谱系数的取值分析   总被引：3，自引：1，他引：2  

朱守红 《时间频率学报》1998,21(2):12-16

精密时钟噪声可用五个幂律谱系数来表征其强弱。由于不存在实际可用的理想时钟作为参考,用以估计幂律谱系数的单钟噪声无法直接测出,而只能利用钟组内各钟之间的钟差。然而这是一个不适定问题．本文探讨了单钟幂律谱系数的取值范围与优化估计方法。  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