QuickBird影像制作1：10000DOM方法探讨

随着卫星遥感影像数据更加广泛地应用于测绘,针对QuickBird影像制作1：10000 DOM的方法,从正射纠正的三种不同方式进行了实验和探讨,分析了利用外业控制点或者在原有DRG、DOM上选取控制点制作DOM的方法、精度、工作量,总结提出了方便、快捷、实用的工作模式。     

数字地质调查中多源地学数据在造山带构造单元 划分和大地构造演化研究方面的应用 ——以青海民和地区为例

多源地学数据包括遥感、地球化学和地球物理数据,介绍了利用多源地学数据进行造山带构造单元划分的方法。遥感数据在确定区域构造边界及活动断层方面的应用非常广泛,遥感影像在解译线形构造即断层方面有非常明显的效果,可以根据不同构造单元的影像差异,区分不同的地质体、线性构造及活动断层,同时用遥感数据叠加三维地形数据分析线性构造可以更加直观地解译线性构造。地球化学数据在确定大的构造边界方面具有一定的指示意义,可以根据水系沉积物的地球化学特点,运用因子分析方法确定大的构造边界。地球物理数据提供的是地质体及构造边界在深部的延伸情况,可以为研究断裂的运动学和动力学特征提供证据。     

中国数字地质调查系统的基本构架 及其核心技术的实现

数字地质调查系统是贯穿整个地质矿产资源调查全过程的软件,涵盖地质矿产调查、矿产资源勘查、矿体模拟、品住估计、资源量估算、矿山开采系统优化等内容。考虑数字地质调查系统的应用技术层面,从数据“层”模型、数据流“池”技术、不同阶段数据模型继承技术、数据互操作技术等几个方面讨论了核心技术及其实现,通过基于无缝一体化技术的数据采集、管理、综合处理与成果表达,在实体或矿块的矿床建模技术与品住估计、储量估算等方面展现了全地质调查过程的数字化,不但为地质人员应用高新技术降低了门坎,而且极大地提高了研究精度和效率,丰富了成果的表现形式和服务形式。随着数字地质调查系统的完善和应用水平的提高,数字地质调查系统将成为中国地质调查的主流软件体系。     

DCT域遥感影像融合算法

提出一种基于离散余弦变换(Discrete Cosine Transform,DCT)与IHS变换的多光谱与全色遥感影像融合方法及其改进算法。本文方法依据DCT系数的特点在DCT域进行遥感影像融合,适合压缩格式的遥感影像快速融合。目视效果与客观评价表明,相比常用遥感影像融合方法,本文方法能在提高空间分辨率与保持光谱特性之间得到更好的折衷。     

测井仪器的故障分析与排除思路

TYSC-3Q与PSJ-2型数字测井仪是目前煤田测井中常用的二种测井仪器,在使用过程中难免发生诸如测井控制故障、声速探管故障、密度三侧向探管故障、井温、井液电阻率探管故障、电法面板故障、数字测井面板故障、电测井故障等常见故障类型。通过对各类故障因素进行剖析,指出了故障易发生的部位,并详细的介绍了检查的方法及故障的排除步骤。     

我国煤炭航测技术的最新发展

中国煤炭地质总局航测遥感局作为我国煤炭航测技术的主要单位,承担着95％以上的煤炭矿区航测成图任务,并逐步发展成为我国集航空摄影、遥感地质、地图制印、地下管线探测、地理信息技术等全面发展的空间信息产业集团：伴随着计算机技术的发展,煤炭航测技术走过了从模拟测图到解析测图,最后发展到今天的全数字测图的历程。目前煤航已拥有和掌握了IMU／DGPS辅助航空摄影技术、SAR（合成孔径雷达）成图技术、LIDAR（机载激光扫描）技术等空间数据采集最新技术。     

Overbreak and underbreak in underground openings Part 2: causes and implications

Summary The newly developed light sectioning method has been used to investigate some of the causes and costs of overbreak and underbreak. Investigations at the Aquamilpa Hydroelectric Project in Mexico have shown decreased overbreak and increased underbreak as a result of increased rock quality and decreased explosive energy. A new measure of explosive energy, the perimeter powder factor (PPF), has been defined and shown to be useful in the context of tunnel-wall rock damage. Tentative results indicate that explosive energy (PPF) may be a more important factor in producing underbreak, whereas rock quality may be a greater factor in producing overbreak. A site-specific equation is given for predicting overbreak or underbreak as a function of rock quality and explosive energy, with an evaluation of the cost of underbreak and overbreak.     

Textural segmentation of digital rock images into bedding units using texture energy and cluster labels

The texture of digital rock images, as recorded, for instance, with borehole imaging devices, is shown to reflect different bedding types. Textural segmentation of borehole images, therefore, subdivides the recorded sequence into bedding units. We show that a textural segmentation algorithm based on the concept of texture energy achieves good results when compared with synthetic as well as real data in which petroleum geologists have performed zonations on cores. Texture energy involves filtering of the original image with a set of texture sensitive masks. The filtering is done as a finite convolution over the size of the masks. On the resulting images the variance is computed over a relatively large sliding window, which, in its practical implementation, covers the full width of the image. The resulting nine one-dimensional curves are then clustered hierarchically into a user-determined number of image texture or lithological bedding classes. Principal component analysis previous to clustering can be used to reduce redundancy in the data. A recurring and relatively ill-defined problem in this field are macro-textures, i.e., the cyclic interbedding of two or more bedding types. We show that sliding Fourier transforms and variable mask scale can successfully address the zonation of macro-textures. In general, the method gives best results with mask sizes equivalent to 2–4 centimeters, reflecting the length scale at which the investigated geological bedding seems to have its highest variation.     

X-ray spectroscopy of stellar coronae

Summary From the early discovery in 1948 of X-rays from the Solar corona, X-ray spectroscopy has proven to be an invaluable tool in studying hot astrophysical and laboratory plasmas. Because the emission line spectra and continua from optically thin plasmas are fairly well known, high-resolution X-ray spectroscopy has its most obvious application in the measurement of optically thin sources such as the coronae of stars. In particular X-ray observations with theEINSTEIN observatory have demonstrated that soft X-ray emitting coronae are a common feature among stars on the cool side of the Hertzsprung-Russell diagram, with the probable exception of single very cool giant and supergiant stars and A-type dwarfs. Observations with the spectrometers aboardEINSTEIN andEXOSAT have shown that data of even modest spectral resolution (/ = 10–100) permit the identification of coronal material at different temperatures whose existence may relate to a range of possible magnetic loop structures in the hot outer atmospheres of these stars. The higher spectral resolution of the next generation of spectrometers aboard NASA'sAXAF and ESA'sXMM will allow to fully resolve the coronal temperature structure and to enable velocity diagnostics and the determination of coronal densities, from which the loop geometry (i.e. surface filling factors and loop lengths) can be derived. In this paper various diagnostic techniques are reviewed and the spectral results fromEINSTEIN andEXOSAT are discussed. A number of spectral simulations forAXAF andXMM, especially high-resolution iron K-shell, L-shell, and2s-2p spectra in the wavelength regions around 1.9 Å, 10 Å, and 100 Å, respectively, are shown to demonstrate the capabilities for temperature, density, and velocity diagnostics. Finally, iron K-shell spectra are simulated for various types of detectors such as microcalorimeter, Nb-junction, and CCD.