分水岭算法在电成像测井图砾石识别中的最优参数研究

基于电成像测井,将分水岭算法应用到电成像测井图砾石的识别中,分水岭算法在砾石识别应用中的参数选取直接影响到识别效果。针对分水岭算法识别砾石的各个步骤,选取不同的优化参数进行处理,对处理效果进行对比分析,最终确定分水岭算法识别砾石的最优参数,并对吉林王府断陷AA井、BB井和CC井三口井进行实际处理,得到很好的效果。     

一种提高储层裂缝识别准确度的方法

油田勘探开发中,储层裂缝的高效、准确识别一直是一个难题。常规测井裂缝识别方法方便但准确度低,电成像测井裂缝识别方法纵向分辨率高、识别准确但人工识别繁琐。为了解决常规和电成像测井裂缝识别方法各自缺点带来的问题,本文提出了一种既高效又准确的储层有效裂缝识别方法。该方法以裂缝在电成像测井上的响应特征为依据,选取裂缝层段为样本,构建常规测井裂缝综合识别因子Y₁和电成像测井裂缝识别因子Y₂,将两因子结合构建储层裂缝识别因子Y₃。利用Y₃识别裂缝,采样点间隔为0.002 54 m,远小于常规测井的0.125 m,比常规测井识别裂缝准确度高;自动拾取裂缝效率远高于繁琐的人工识别,比电成像测井识别裂缝省时省力。将该方法应用到王府地区火山岩储层裂缝识别中可快速准确地识别储层裂缝,准确率达到80%左右,对其他类型储层裂缝研究有一定的借鉴意义。     

基于超声波合成孔径技术的钻孔成像方法

随着地下空间开发的深入,钻孔岩壁上特殊区域的重视程度越来越高,为了克服传统超声波钻孔成像技术分辨率低的不足,提出一种基于超声波合成孔径技术的钻孔成像方法,提高钻孔图像的分辨率和图像质量。采用高分辨率的合成孔径SAFT成像技术综合处理大量的断面扫描回波信号,达到增强反射信号和抑制干扰信号的目的,使对应的岩壁特征区域回波更加突显,在该基础上提取出扫描断面回波信号的声幅和声时参数。综合声幅和声速参数的特征,提出了基于相关性的超声波钻孔图像重建原则,选择合适的成像数据点,在叠加不同深度的探测数据后形成了关注区域更加明显的钻孔重建图像。将该方法应用到了实际工程中,验证了该方法的可行性和准确性。     

钻孔雷达反射成像在岩溶发育场地探测中的应用

我国岩溶区分布广泛,且复杂的岩溶现象对建筑安全、地基稳定以及场地勘察有较大影响。钻孔雷达作为一种井中地球物理方法,可以利用地下介质的物性差异查明岩溶发育的情况,弥补常规勘察手段在探测岩溶发育场地中存在的不足。依据钻孔雷达单孔反射信号的同相轴特征、反射波首波走时和反射波的衰减等特征,可判断钻孔周边未揭露溶洞和裂隙的分布,确定钻探揭露溶洞的水平方向直径以及岩石完整性,从而达到查明各种岩溶形态的规模、空间密度及其分布规律的目的,为工民建各项工程建设的设计和施工提供准确详尽的地质资料,确保工程的稳定性。      

Near-nucleus imaging of comet IRAS-Araki-Alcock 1983H1

Several digital image processing techniques were used to improve the visibility of details, fans and jets, in the inner coma of the comet IRAS-Araki-Alcock 1983 VII on the short CCD-exposures taken by R. E. Schild with the 61-cm telescope through three I, J, and F band filters, at the Whipple Observatory during the close approach from May 6 through May 12, 1983. About 140 CCD images with the pixel size of 0.73 give a resolution about 20 km, and selected CDD frames presented together with isophotes demonstrate the variation and interrelation of the coma morphology and the nucleus activities during the observing period. Results and processed images are compared with observations taken by other observers during the same period.     

Hard X-ray imaging via focusing optics with mosaic crystals

In spite of the tremendous potential of hard X-ray astronomy (>10 keV) for studying high energy phenomena in celestial objects, the current generation of direct-viewing telescopes is heavily noise limited. It can accurately study only the strongest sources. Thus focusing of hard X-rays is mandatory in order to overcome these sensitivity limitations. Several focusing techniques of hard X-rays (>10 keV) are under study. We will discuss the Bragg diffraction technique and the imaging performance of a concentrator configuration based on this technique. Apart from its unprecedented flux sensitivity, the Bragg concentrators show intrinsic capabilities as polarimeters.     

The university of New South Wales automated patrol telescope

The Automated Patrol Telescope is a wide-field CCD imaging telescope of novel design. The telescope is a converted Baker-Nunn satellite tracking camera that has undergone extensive modification to its optical, mechanical and electronic systems. Telescope operation is entirely under computer control, and the instrument is to be used for a variety of astronomical survey and monitoring projects.     

Ska and Evla Computing Costs for Wide Field Imaging

I investigate the problem of high dynamic range continuum synthesis imaging in the presence of confusing sources, using scaling arguments and simulations. I derive a quantified cost equation for the computer hardware needed to support such observations for the EVLA and the SKA. This cost has two main components – from the data volume, scaling as D⁻⁶ (where D is the antenna diameter), and from the non-coplanar baselines effect, scaling as D⁻², for a total scaling of D⁻⁸. A factor of two in antenna diameter thus corresponds to 12 years of Moore’s law (18 month doubling time) cost reduction in computing hardware. For a SKA built with 12.5 m antennas observing with 1 arcsecond at 1.4 GHz, I find the computing load to be about 150 Petaflops (costing about $500 million in 2015). For 25 m antennas, the load is about 256 times lower, costing $2 million in 2015. This new cost equation differs from that of Perley and Clark (2003), which has scaling as D⁻⁶. This is because I find that the excellent Fourier plane coverage of the small antenna design does not significantly change the convergence rate of the Clean algorithm, which is already satisfactory in this regime.The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation.     

显微CT的发展及其对美容-保健的影响

本文评述美国五家公司的显微CT（以下简称MCT）的现状和发展趋势,在颅凳面病人实际行皮肤切片,显示薄层细胞的基础上,结合MCT做二维和三维的CT成像,成立体,详尽和精确地显示皮肤表层5－10毫米,机体组织三维解剖结构,包括表皮,真皮、脂肪、动脉、静脉的空间分布及其相互关系,探讨显微CT和螺旋CT机在其成像分辨率提高的进程,再现美容病体模型的程度可达到亚微米级的精度,为掌握病情并制定合理的手术计划提供了重要依据,提高－整形的效果,实现全方位扫描和精密三维重建技术在颅凳面皮肤美容和减肥的适应症的应用价值。结果：显微CT三维重建技术是现代皮肤美容和保健的主要诊断方法之一,并具有重要的临床应用价值;近年来工业微焦点CT机其空间分辨率已达5－15微米,已发展了用于生物医学的研究,今后对可皮下组织作精细的CT成像,以了解形整美容,减肥,对当前的美容和保健产品给予在亚微米级,从细胞发育情况的定量评价,表述其CT影像的微观结果。     

电阻率层析成像及演中若干问题的讨论

以双异性点电流源电流场二维地电断面为例，着重讨论了电阻率展析成像反演中有限单元法数值模拟边界条件的选择、网格剖分以及模拟精度等问题，同时也讨论了成像反演中最优化及演方法及拟合参数的评价等。文中提出的新的网格剖分方法和选择的边界条件可有效地提高计算速度和数值模拟的精度。