随钻方位电磁波电阻率成像模拟及应用

随钻方位电磁波电阻率成像资料在地质导向中起着至关重要的作用。利用三维有限差分数值模拟方法计算随钻电阻率仪器激发的电磁场随仪器方位变化的规律,分析实现方位电阻率测量以及成像的原理及方法。数值模拟结果表明：在常规随钻电磁波仪器的基础上,增加倾斜或横向接收(发射)天线,可以实现地层方位的预测和判断,同时方位电磁波电阻率成像结果受相对井斜角、地层电导率对比以及地层地质构造的影响;利用方位电阻率成像以及定向信号成像结果可以预测和判断层界面、地层方位特征以及各向异性地层走向;幅度比电阻率成像效果优于相位差电阻率成像;在均匀各向异性介质中,线圈距和工作频率越大,视电阻率受垂向电阻率影响越大;线圈距越大,定向幅度信号越强,能预测的层界面的距离越大。     

Review of research on sonar imaging technology in China

Over the past 20 years, sonar imaging technology particularly for the high-technology sector has been a focus of research, in which many developed countries, especially those with coast lines, have been competing with each other. It has seen a rapid development with increasing widespread applications that has played an important and irreplaceable role in underwater exploration with great prospects for social, economic, scientific, and military benefits. The fundamental techniques underlying sonar imaging, including multi-beamforming, synthetic-aperture and inverse synthetic-aperture sonar, acoustic lensing, and acoustical holography, are described in this paper. This is followed by a comprehensive and systematic review on the advantages and disadvantages of these imaging techniques, applicability conditions, development trends, new ideas, new methods, and improvements in old methods over recent years with an emphasis on the situation in China, along with a bold and constructive prediction to some development characteristics of sonar imaging technology in the near future in China. The perspectives presented in this paper are offered with the idea of providing some degree of guidance and promotion of research on sonar imaging technology.     

基于多波束测深系统的水下成像技术

为实现多波束测深系统的一体化探测功能,研究分析了利用快拍法进行多波束水下成像的基本原理,并考虑实际中的水声环境和多波束测深系统自身的复杂性,对用于成像的位置数据和散射强度数据进行了修正,湖上试验数据的处理结果表明了该方法对水中目标的探测能力,验证了其工程应用的可行性。     

小脑星形细胞瘤的MRI诊断

目的探讨小脑星形细胞瘤的MRI表现,提高对本病的诊断水平.方法回顾性分析经手术及病理证实的31例小脑星形细胞瘤的MRI资料. 结果实质瘤体型7例,瘤在囊内型10例,囊在瘤内型13例,1例表现为完全囊性,31例均表现不同程度的梗阻性脑积水表现. 结论小脑星形细胞瘤具有特征性,增强扫描有助于病灶检出和定性诊断.术前诊断是可能的,但需与血管母细胞瘤、髓母细胞瘤、室管膜瘤、转移瘤相鉴别.     

Differential rotation on both components of the pre-main-sequence binary system HD 155555

We present the first measurements of surface differential rotation on a pre-main-sequence binary system. Using intensity (Stokes I) and circularly polarized (Stokes V) time-series spectra, taken over 11 nights at the Anglo-Australian Telescope (AAT), we incorporate a solar-like differential rotation law into the surface imaging process. We find that both components of the young, 18 Myr, HD 155555 (V824 Ara, G5IV + K0IV) binary system show significant differential rotation. The equator–pole lap times as determined from the intensity spectra are 80 d for the primary star and 163 d for the secondary. Similarly, for the magnetic spectra we obtain equator–pole lap times of 44 and 71 d, respectively, showing that the shearing time-scale of magnetic regions is approximately half of that found for stellar spots. Both components are therefore found to have rates of differential rotation similar to those of the same spectral-type main-sequence single stars. The results for HD 155555 are therefore in contrast to those found in other, more evolved, binary systems where negligible or weak differential rotation has been discovered. We discuss two possible explanations for this: first that at the age of HD 155555 binary tidal forces have not yet had time to suppress differential rotation and secondly that the weak differential rotation previously observed on evolved binaries is a consequence of their large convection zone depths. We suggest that the latter is the more likely solution and show that both temperature and convection zone depth (from evolutionary models) are good predictors of differential rotation strength. Finally, we also examine the possible consequences of the measured differential rotation on the interaction of binary star coronae.     

The Solar Dynamo and Its Phase Transitions during the Last Millennium

Variations in total solar irradiance (TSI) correlate well with changes in projected area of photospheric magnetic flux tubes associated with dark sunspots and bright faculae in active regions and network. This correlation does not, however, rule out possible TSI contributions from photospheric brightness inhomogeneities located outside flux tubes and spatially correlated with them. Previous reconstructions of TSI report agreement with radiometry that seems to rule out significant “extra-flux-tube” contributions. We show that these reconstructions are more sensitive to the facular contrasts used than has been generally recognized. Measurements with the Solar Bolometric Imager (SBI) provide the first reliable support for the relatively high, wide-band, disk-center contrasts required to produce 10% rms agreement. Longer term bolometric imaging will be required to determine whether the small but systematic TSI residuals we see here are caused by remaining errors in spot and facular areas and contrasts or by extra-flux-tube brightness structures such as bright rings around sunspots or “convective stirring” around active regions.     

基于积分视场单元的三维天文成像光谱技术

近年来,三维成像光谱技术主要是发展和采用积分视场单元方法,即将枧场内的展源目标连续切割成若干单元,重新排列后进入光谱仪器,同时获得展源的高分辨率三维数据立方体(x,y和λ).相对于传统的技术方法,这种基于积分枧场单元的三维成像光谱技术进行一次观测可以同时获取天体各处的二维空间信息和光谱信息.采用积分视场单元虽然在光谱数据处理上会带来很多困难,但由于其在观测时间和效率上具有明显的优点,因此值得采用.该文简要介绍了三维成像光谱技术的原理;评述了目前实现三维成像光谱的三种不同类型的技术系统:小透镜阵系统、光纤加小透镜阵系统、像切分器系统,重点介绍了像切分器系统的有关情况;最后展望了三维成像光谱技术在天文学上的应用.     

多功能超声波成像测井仪应用效果评价

多功能超声成像测井仪采用超声脉冲反射法进行套损及水泥胶结质量评价.对该仪器实测的波形进行分析,波形信噪比良好,首波为套管内壁的反射波,随后到达的为套管共振波,波形频谱曲线具有明显的谱陷特征.利用井眼内壁反射波的幅度及到时曲线可实现井眼内壁高分辨率成像;利用套管共振波的共振频率及幅度衰减可分别计算套管厚度及套管后面材料的水泥声阻抗.现场实测的裸眼井资料表明,该仪器可获取井壁表面裂缝、层理、孔洞等地质构造信息.处理现场实测的套管井资料表明,仪器可正确测量套管的壁厚,识别套损方位,同时还可以根据水泥声阻抗的数值范围确定一界面材料是气体、液体还是固体成分.该仪器具有井眼内壁成像、套损评价及水泥胶结质量评价的功能.     

基于单程波方程的角度域保幅偏移(英文)

传统叠前深度偏移只能够提供地下的构造信息,但工业界在需要构造信息的同时还要与地下界面反射系数成比例的振幅信息。最近几年,基于单程波方程的保幅叠前深度偏移算法有了一定的发展,但是,基于炮域、单程波的保幅型叠前深度偏移必须应用反褶积型的成像条件,这种成像条件在构造复杂、速度变化剧烈的地区会出现不稳定现象。基于角度域的保幅深度偏移克服了这一不稳定性缺点的同时,还域的保幅深度偏移,模型和实际资料的试算分析验证该思路方法的正确性和有效性。     

小波方法在地电场干扰处理中的分析研究

该文在对地电场信号及地电阻率人工供电干扰信号的时频特征进行分析的基础上, 提出了小波域阈值滤波方法, 对地电场秒采样信号中叠加地电阻率人工供电干扰信号进行了分析和处理, 处理产生的误差在地电场观测的允许误差范围之内。