激光跟踪仪测量精度的评定

介绍了影响激光跟踪仪测量精度的各种因素及对其测量精度进行评定的意义、指标及方法,阐述了比较法在仪器现场检查和校准中的应用,并以100MeV直线加速器的测量控制网为例,说明统计分析法在验后精度评定中应用。     

基于激光跟踪仪的三维控制网测量精度分析

介绍三维控制网的优点及激光跟踪仪测量系统的特点,讨论了光束法平差原理及不同观测值的权比问题,并以100MeV电子直线加速器安装测量控制网的模拟计算和实测结果,论证了利用激光跟踪仪进行三维控制网的精度。     

基于GPS激光主动式定位系统定位方法研究

介绍了GPS激光主动式定位系统的硬件组成及功能,分析了该方法定位的基本原理,并对试验结果进行了分析,验证该方法的可行性及定位精度。利用系统在不同的流动站对目标利用系统同轴望远镜进行照准,发射激光获取不同流动站的距离,利用数字罗盘获取激光仪的姿态,GPS_OEM获得流动站点的GPS坐标。利用空间距离交会原理解算目标的3维坐标,为不易到达的测区提供技术方法。     

基于地物特征提取的车载激光点云数据分类方法

车载激光扫描测量方法较传统摄影测量方法具有更多优点,它能快速采集大面积、高精度的三维空间数据,具有广阔的应用前景。针对车载激光扫描数据的分类问题,提出了一种基于地物特征提取的点云数据分类方法,即采用主成分分析(PCA)方法,在提取多种街区地物点云数据几何特征和总结地物对象特征知识规则的基础上,根据选取的主特征设计一套阶层式的分类方法,并利用该方法对一套车载激光点云数据进行了分类试验。结果表明,该方法的分类效果良好,具有一定的实用性。     

大型制像工程分块壁板测量方法

一般大型制像工程要经过小比例模型(1∶10)、1∶1石膏模型及艺术重塑、分块壁板铸造与室内预组装、现场安装等工艺流程。阐述由1∶1石膏模型到现场安装的成型测绘技术,包括大型制像工程中分块壁板的结构特点、安装技术要求、测量安装定位方法以及建造过程中所涉及的测量技术要求等,并以在建的某48m大佛头部安装为工程实例,详细阐述分块壁板测绘、室内预组装、现场安装的测控技术流程,评定石膏模型分块角点的测量精度。进而,总结出一套适于大型制像工程的测绘技术和方法,为同类制像工程提供借鉴和帮助。     

目标颜色和入射角对Trimble GX扫描点云精度的影响

介绍三维激光扫描仪的误差分类及近年来国外在目标反射特性对点云精度影响方面的研究进展,大量实验表明点云精度与目标表面反射特性存在较强关系。通过对纸质贴片点云分析得出如下结论:Trimble GX三维激光扫描仪所测点云标准偏差与反射激光亮度符合乘幂函数关系;目标颜色对该扫描仪测量精度有较大影响,白、绿、黄、蓝等颜色对绿色激光反射率较好;纸质贴片旋转一个较小角度可使扫描点云质量最优;纸质贴片反射特性服从朗伯余弦定律。     

The C1XS X-ray Spectrometer on Chandrayaan-1

The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray spectrometer for the Indian Space Research Organisation (ISRO) Chandrayaan-1 lunar mission. It exploits heritage from the D-CIXS instrument on ESA's SMART-1 mission. As a result of detailed developments to all aspects of the design, its performance as measured in the laboratory greatly surpasses that of D-CIXS. In comparison with SMART-1, Chandrayaan-1 is a science-oriented rather than a technology mission, leading to far more favourable conditions for science measurements. C1XS is designed to measure absolute and relative abundances of major rock-forming elements (principally Mg, Al, Si, Ca and Fe) in the lunar crust with spatial resolution ?25 FWHM km, and to achieve relative elemental abundances of better than 10%.     

Lunar Prospector measurements of secondary electron emission from lunar regolith

We present the first in situ measurements of the secondary electron emission efficiency of lunar regolith, utilizing Lunar Prospector measurements of secondary electrons emitted from the negatively charged night side and accelerated upward by surface electric fields. By comparing measurements of secondary currents emitted from the surface and incident primary electron currents, we find that the secondary yield of lunar regolith is a factor of ∼3 lower than that measured for samples in the laboratory. This lower yield significantly affects current balance at the lunar surface and the resulting equilibrium surface potentials. This information must be folded into models of the near-surface plasma sheath, in order to predict the effects on dust and other components of the lunar environment, and ultimately determine the importance for surface exploration and scientific investigations on the Moon.     

Quasi-critical orbits for artificial lunar satellites

We study the problem of critical inclination orbits for artificial lunar satellites, when in the lunar potential we include, besides the Keplerian term, the J ₂ and C ₂₂ terms and lunar rotation. We show that, at the fixed points of the 1-D averaged Hamiltonian, the inclination and the argument of pericenter do not remain both constant at the same time, as is the case when only the J ₂ term is taken into account. Instead, there exist quasi-critical solutions, for which the argument of pericenter librates around a constant value. These solutions are represented by smooth curves in phase space, which determine the dependence of the quasi-critical inclination on the initial nodal phase. The amplitude of libration of both argument of pericenter and inclination would be quite large for a non-rotating Moon, but is reduced to <0°.1 for both quantities, when a uniform rotation of the Moon is taken into account. The values of J ₂, C ₂₂ and the rotation rate strongly affect the quasi-critical inclination and the libration amplitude of the argument of pericenter. Examples for other celestial bodies are given, showing the dependence of the results on J ₂, C ₂₂ and rotation rate.     

The sensitivity of the next generation of lunar Cherenkov observations to UHE neutrinos and cosmic rays

We present simulation results for the detection of ultra-high energy (UHE) cosmic ray (CR) and neutrino interactions in the Moon by radio-telescopes. We simulate the expected radio signal at Earth from such interactions, expanding on previous work to include interactions in the sub-regolith layer for single dish and multiple telescope systems. For previous experiments at Parkes, Goldstone (GLUE), and Kalyazin we recalculate the sensitivity to an isotropic flux of UHE neutrinos. We find the published sensitivity for the GLUE experiment to be too high (too optimistic) by an order of magnitude, and consequently the GLUE limit to be too low by an order of magnitude. Our predicted sensitivity for future experiments using the Australia Telescope Compact Array (ATCA) and the Australian SKA Pathfinder (ASKAP) indicate these instruments will be able to detect the more optimistic UHE neutrino flux predictions, while the square kilometre array (SKA) will also be sensitive to all bar one prediction of a diffuse ‘cosmogenic’, or ‘GZK’, neutrino flux.Outstanding theoretical uncertainties at both high-frequency and low-frequency limits currently prevent a reliable estimate of the sensitivity of the lunar Cherenkov technique for UHE cosmic ray (CR) astronomy. Here, we place limits on the effects of large-scale surface roughness on UHE CR detection, and find that when near-surface ‘formation-zone’ effects are ignored, the proposed SKA low-frequency aperture array could detect CR events above 56 EeV at a rate between 15 and 40 times that of the current Pierre Auger Observatory. Should further work indicate that formation-zone effects have little impact on UHE CR sensitivity, observations of the Moon with the SKA would allow directional analysis of UHE cosmic rays, and investigation of correlations with putative cosmic ray source populations, to be conducted with very high statistics.