双平方根波动方程偏移速度分析

传统的剩余校正（RMO）偏移速度分析方法基于走时原理,在陡倾角和欠照明地区,因为不能得到充分的角度域信息而失效.本文将展示一种基于波场延拓理论的偏移速度分析方法,即波动方程偏移速度分析（WEMVA）.这种方法先利用成像优化方法获得剩余成像,再利用剩余成像反演剩余速度.此类方法继承了波动方程偏移方法的优点和缺点.波动方程偏移速度分析是一种线性反演方法,它要求对Born近似的展开序列作一阶截断.高阶部分的丢失必然带来巨大的截断误差,因此剩余成像必须也进行线性化,以适应大速度扰动和大延拓步长.因此,在此类算法中,剩余成像的获取和线性化是偏移速度分析的关键.在叠前偏移算子中,因为双平方根算子的数学表达式更为简洁,所以本文基于对波动方程偏移速度分析初步讨论,并通过模型验证其原理.     

利用联合反演技术进行反射地震的波速成象

本文介绍了根据反射地震数据进行波速成象的一种方法,其基础为多种反演技术的综合。由于要求的波速图象C（x,z）具有间断性,除利用走时数据T（x,t）外,在地层比较水平的情况下,还利用了均方根速度V（x,t）和统计子波W（t）的数据来成象。计算机层析成象过程分为三步:首先重做速度分析,取得与初次反射走时一致的均方根速度数据;然后用反射走时与均方根速度联合反演对应分析道的层速度和界面深度;最后由联合反演结果和反射面走时求波速图象函数的数字化版。文中还给出了波速成象方法在我国西北某沉积盆地上的应用及验证结果。     

支气管囊肿外科治疗36例临床分析

纵隔型支气管囊肿（MBC）是一种先天性支气管囊肿,多发生于中纵隔中上部,发生在后下纵隔相对少见。本文报道1例后下纵隔支气管囊肿患者,19岁,男性,体检发现纵隔占位。CT表现为后下纵隔脊柱旁不规则肿块,密度混杂,边缘及内部可见结节状钙化,增强后未见强化。MRI检查T1WI呈不均匀低信号,T2WI呈高信号,内见条索状、分隔样低信号,增强后延迟期病灶边缘及分隔轻度强化。术后病理诊断：支气管源性囊肿。本文回顾性分析该病例的CT和MRI影像特征,并复习国内外文献,总结后下纵隔不典型支气管囊肿的影像表现,以提高对该疾病的认识。

     

基于粗糙集和遗传算法的超光谱波段集合整体缩减

提出一种对高光谱遥感影像波段集合进行整体缩减的方法。该方法首先根据模糊集和粗糙集理论,对原光谱波段集会进行近似等价波段区间的自动划分。对于每个近似等价波段区间,在考虑其他区间合成影像数据影响的情况下,利用遗传算法进行合成权系数的优化。实验表明,整体迭代线性合成方法不仅具有较高的计算效率,而且可以获得比独立线性合成方法明显优化的结果。     

二维介质柱的电磁成像研究

从体等效原理出发得到用介质柱介电参数表示的体等效电流,并得到一个积分方程组求解散射问题．利用变分原理,对此方程组求变分,并化为矩阵方程组,消去含介质柱内总场变化的项,得到散射场变化与介质柱介电参数变化之间关系的矩阵方程．即反演方程．用算例检验此法的反演精度、收敛性能、多目标反演能力、抗噪声性能及利用不完备测量散射信息反演目标的能力．结果表明,此法是一种实用性很强的二维介质柱电磁成像方法．     

多导体柱微波成像的连续编码遗传算法

提出一种能同时重建多个二维良导体目标外形轮廓的新方法——连续编码遗传算法．将目标的横截面轮廓近似表达为三角级数形式,由边界条件得到一积分方程组,在此基础上将成像问题转化为约束优化问题,级数的各项系数为待优化量．积分方程组为约束条件,目标函数定义为实际测量的散射场与反演过程中得到的散射场之间的相对误差函数．采用连续编码遗传算法求解,优化过程通过选择、交叉、变异等遗传操作的选代而实现,待优化目标函数进行线性变换并采用模拟退火原理确定目标后表达为适应度函数,采用联赛选择与比例选择相结合的选择机制和单点交叉方式,变异操作通过对基因施加微小随机扰动实现．上一代中适应度最高的个体直接保留．数值模拟反演实验验证了方法的有效性．与其他反演方法相比,本法具有简单、通用、鲁棒性强等特点．     

Sharp images of young stellar objects

We present high resolution infrared images of the pre-main sequence star V536 Aql and polarization maps of the reflection nebula IRN Cha observed with the SHARP camera on the ESO NTT. Extended structures are observed near V536 Aql. The polarization pattern of IRN Cha is typical of a centrally illuminated source but with a central band of anomalously oriented polarization believed to occur in an optically thick disk.     

Rapid delineation of subsurface petroleum contamination using the site characterization and analysis penetrometer system

 The Site Characterization and Analysis Penetrometer System (SCAPS) was used to investigate subsurface petroleum contamination at Aberdeen Proving Ground, Maryland. The SCAPS is a rapid site-screening tool developed by the Tri-Services (U.S. Army, Navy, and Air Force) to reduce the cost of installation restoration activities. The system, consisting of a geophysical cone penetrometer fitted with a laser-induced fluorescence petroleum sensor, is capable of simultaneous, real-time delineation of subsurface stratigraphy and petroleum contamination. Onsite processing of the SCAPS data allows three-dimensional visualization of both subsurface stratigraphy and petroleum contaminant distribution. The site investigation described herein successfully identified three distinct areas of subsurface petroleum contamination caused by leaking underground storage tanks containing No. 2 healing oil. The SCAPS petroleum sensor response was verified by obtaining 20 soil samples and performing onsite and conventional laboratory analyses for petroleum contaminants. Verification sample results indicate a strong correlation between the SCAPS fluorescence data and conventional measures of petroleum contamination. This investigation illustrates the capabilities of the SCAPS for rapid site characterization. Received: 27 November 1995 · Accepted: 11 December 1995     

Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg

We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near-Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1-year period found in the radial velocity measurements for this star. We can model the time-dependent asymmetry either as the orbit of a low-mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3-year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 ± 0.1 D _* full width at half-maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 ± 0.3. While the most likely explanation for the 20 per cent change in brightness is non-radial pulsation, we argue that a low-mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low-mass companion could explain the behaviour revealed by the radial velocity curves and the time-dependent asymmetry detected in the closure-phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low-mass companion on the primary star.