Application of laser strainmenters to the study of earthquake physics

The paper considers possibilities of applying laser strainmeters for the study of earthquake physics. One of laser strainmeters is described. A high efficiency of using the laser strainmeters for the study of earthquakes and their precursors is shown. In records of the spaced laser strainmeters, anomalous deformations propagating from the east to the west with the speed comparable with that of migration of earthquakes were found.     

松辽盆地地浸砂岩型铀矿勘查及其找矿方向

20世纪90年代开始,在松辽盆地开展了地浸砂岩型铀矿区域评价工作.盆地的西南部投入数万米钻探工作量开展以第三系和上白垩统嫩江组、姚家组为目的层的找矿工作,取得了较大突破,发现并提交了我国第一个板状砂岩型铀矿床,所建立的双混合叠造铀成矿模式丰富了地浸砂岩型铀成矿理论.在此基础上总结出白垩系砂岩型铀成矿控矿因素和找矿标志.盆地东部构造反转有利于形成砂岩型铀矿床.第三系以潜水氧化为主,还原物质缺乏,而且新构造运动对其改造微弱,总的成矿条件不理想,不宜作为主攻目的层.盆地坳陷阶段沉积的泉头组、青山口组、姚家组为主要找矿目的层,找矿重点在盆地东南部通辽-双辽-德惠地区.下一步科研工作重点为:完善QJD砂岩型铀矿模式、盆地油气与铀成矿关系、白垩纪古水文地质条件的研究.     

太空垃圾实时监测系统建立可行性分析

介绍了太空垃圾监测及清除工作现状,分析了现有监测太空垃圾的雷达技术、激光技术及激光雷达技术的可行性,以STK软件模拟分析太空垃圾运动轨迹,得出了太空垃圾实时监测系统的可实现方法和建议。     

陕西马元地区铅锌矿地质特征及找矿远景

陕西马元地区铅锌矿位于扬子地台北缘碑坝隆起东南缘一带。矿化带长大于60km,宽10～200m,可分为南、东、北3个铅锌矿化带,已圈出了40多条铅锌矿体。其中南矿化带长大于20km,宽20～120m,已圈出了40多条铅锌矿体;东矿化带长大于30km,宽20～200m,地表已发现7条铅锌矿体;北矿化带长大于10km,宽10～100m。矿体一般长100～2560m,厚0.80～10.01m,锌品位1.05%～10.82%,铅品位0.55%～7.54%。主矿体长2560m,厚1.46～32.53m,平均厚约7.60m,最厚28.40m,锌品位1.45%～11.42%,平均4.47%。矿化带主体由震旦系灯影组白云岩组成,产于灯影组的砾状白云质角砾岩带中。矿化主要受地层和构造的控制。经预测,马元地区铅锌矿有较好的找矿远景,具有形成超大型铅锌矿的潜力。     

Laser Scanning的基本原理及其应用前景

首先介绍了激光测距仪的发展历程,针对应用领域的不同,分别对3维激光成像仪和机载/星载激光测高仪的测量原理进行了阐述,并分别介绍了两种激光测距仪的工作流程以及数据处理流程,最后对两种激光测距仪的应用范围进行了阐述,并把两种激光测距技术和普通摄影测量进行了比较,指出了激光测距技术相对于普通摄影测量的优点,即高精度性、穿透性、实时性。     

基于BP神经网络的三维激光测高数据拟合方法

针对三维激光测高拟合问题，本文采用BP神经网络进行拟合，该方法可以有效地消除或减弱数据中的系统误差影响，提高计算精度。实际算例证明，在数据无粗差情况下，BP神经网络的内符合与外符合精度优于传统的二次曲面拟合的精度。     

一种应用于城市区域的自适应形态学滤波方法

数学形态学滤波是从激光雷达数据中识别地面点、创建数字高程模型的一种重要方法,在应用中取得了较好的效果,但也具有一些明显不足。在分析现有方法优劣及城市地形特点的基础上,提出一种应用于城市环境的自适应形态学滤波算法。该方法采用分层识别策略：首先通过分割得到地面主体部分;之后利用正规化高度值寻找其余地面区域;最后估计地物覆盖区域地面点取值。采用三个不同分辨率、不同地形/地物特点的数据集进行了实验,结果表明该方法能有效识别地面和地物点,并解决了窗口尺寸限制、粗差误判等问题。     

HST colour–magnitude diagrams of six old globular clusters in the LMC

We report on HST observations of six candidate old globular clusters in the Large Magellanic Cloud (LMC): NGC 1754, 1835, 1898, 1916, 2005 and 2019. Deep exposures with the F555W and F814W filters provide us with colour–magnitude diagrams that reach to an apparent magnitude in V of ∼25, well below the main-sequence turn-off. These particular clusters are associated with significantly high LMC field star densities and care was taken to subtract the field stars from the cluster colour–magnitude diagrams accurately. In two cases there is significant variable reddening across at least part of the image, but only for NGC 1916 does the differential reddening preclude accurate measurements of the CMD characteristics. The morphologies of the colour–magnitude diagrams match well those of Galactic globular clusters of similar metallicity. All six have well-developed horizontal branches, while four clearly have stars on both sides of the RR Lyrae gap. The abundances obtained from measurements of the height of the red giant branch above the level of the horizontal branch are 0.3 dex higher, on average, than previously measured spectroscopic abundances. Detailed comparisons with Galactic globular cluster fiducials show that all six clusters are old objects, very similar in age to classical Galactic globulars such as M5, with little age spread among the clusters. This result is consistent with ages derived by measuring the magnitude difference between the horizontal branch and main-sequence turn-off. We also find a similar chronology by comparing the horizontal branch morphologies and abundances with the horizontal branch evolutionary tracks of Lee, Demarque &38; Zinn. Our results imply that the LMC formed at the same time as the Milky Way Galaxy.     

A search for high-velocity gas in massive star formation regions

From the IRAS-PSC, 97 sources with steep FIR spectrum and another 8 were chosen for a search for high-velocity gas. Observations of the CO (J =1−0) line were made with the 13.3-m telescope at the Qinghai Station. The results show that 102 sources are associated with molecular gas. 9 of the sources have reference position problem and 21 have multiple spectrum. Of the remaining 72, 29 contain high-velocity gas, and of these 18 are new molecular outflow candidates. Their properties are discussed briefly in connection with massive young stellar objects.     

激光法气相合成纳米Si/C/N复相粉体

用大功率５ｋＷＣＯ２激光器为能源,以六甲基二硅胺烷［（ＣＨ３）３Ｓｉ］２ＮＨ（简称ＨＭＤＳ）和ＮＨ３为原料,合成纳米非晶Ｓｉ／Ｃ／Ｎ复相粉体。研究了ＨＭＤＳ流量和ＮＨ３对纳米复相粉体组成的影响。ＮＨ３的加入可以大幅度降低纳米复相粉体的碳含量,提高氮含量。Ｓｉ／Ｃ／Ｎ纳米复相粉体的粒径分布范围为１０～５０ｎｍ,为非晶态。