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.     

内核地球自转动力学理论的研究进展(Ⅳ)——内核自转动力学方程

本文是序列文章的第四篇,其内容包括：基于连续介质力学的基本理论,给出了固体外核（SIC）自转的动力学方程,考虑了地球的自引力、液核对内核边界的压力和二阶外部引潮力位对SIC自转的影响,并在O(mε)的量级上给出了其实用的表达式.本文的理论推导更加严密和细致,改正了文献〔1〕在推导过程中的某些错误（例如：（B39）、（B44）和（B59c）式）.本文的工作是对文献〔1〕有关理论的扩展和改进,对进一步研究内核地球自转的动力学理论是非常重要的.     

A high speed near infrared photometer for lunar occultation studies

A recently developed near infrared high speed photometer intended for lunar oc-cultation studies is described. The primary scientific objective is to reach milli arc second levels of angular resolution so that circumstellar structure of the occulted sources can be resolved. Near infrared sky brightness close to the lunar limb is also studied. Angular diameter derived from the observed occultation of IRC +20169 is presented and system performance discussed.     

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.     

DB16智能大型岩土工程无损检测仪及其应用

介绍一种智能大型岩土工程无损检测仪及其应用。该仪器以大功率稀土超磁致伸缩换能器作震源，以与计算机并行接口连接的高速数据传输的16通道DB16数据采集系统进行声波采集，以高灵敏度的低频压电陶瓷(PZT)换能器作接收，用声波层析成像(CT)技术进行数据处理，检测结果用彩色等高图表示。该仪器从参数的设置到数据的采集、保存、CT数据的处理、CT成像等全在一专用软件中完成，操作方便快捷。给出了利用本仪器对某大型水库的泄流深孔挑流鼻坎混凝土浇注质量无损检测的应用实例。     

利用方向纹理特征从影像上搜索道路中心线

针对遥感影像道路中心线提取问题,提出利用方向纹理特征辅助道路中心线匹配搜索的思想,以人工给出的道路种子点和初始搜索方向为基础,运用方向纹理特征直接从遥感影像上匹配搜索道路的中心线。算法通过预测道路的宽度、弯曲等情况来自动调整纹理窗口的大小,因而能够很好地搜索到道路中心线,此外算法针对树木遮挡、车辆压盖设计了相应的处理策略。实验表明:该方法对遥感影像上不同类型道路均有很好的提取效果,且提取效率高于现有的道路提取算法。     

天球有效大气角动量中的周年和半年项估计

为了讨论大气对非刚体地球章动周年和半年项的贡献,本文将大气有效角动量(1980.0～1998.33)从地面参考系转换至空间参考系得到大气的天球有效角动量CEAM,低通滤波后用最小二乘方法拟合得到顺、逆向周年和半年项的振幅估计。     

海洋平台结构超声相控阵检测成像技术的发展及应用

介绍了超声相控阵检测成像技术的基本原理及其在海洋平台结构检测中的最新进展。超声相控阵技术采用区域划分法将焊缝分成垂直方向的若干区,由扫查器携带超声相控阵探头运动,对其分区进行电子扫查,检测结果以图像形式显示。探讨了超声相控阵技术用于海洋平台结构管节点焊缝检测时存在的一些问题,提出解决方法,指出其在海洋平台结构、压力容器、航空航天等工业无损检测领域将具有应用前景。     

大气对地球自转参数（ERP）的高频激发

本文采用１９８３—１９９２年期间由空间大地测量技术观测和归算的地球自转参数（ＥＲＰ）序列，以及由全球气象资料归算的大气角动量（ＡＡＭ）序列，分析和研究了大气对地球自转参数的日长变化（ＬＯＤ）和极移（ｘ和ｙ）在一个月时间尺度以内的高频激发作用，得到的主要结果如下：１大气对ＬＯＤ分量高频潮汐的估计值存在着影响，但是，潮汐形变参数ｋ／ｃ随时间和频率的变化却是受非大气因素的扰动引起的．２．大气可以解释３０天以下ＬＯＤ非潮汐的大部分变化．３．极移分量３０天以内的高频变化也主要由大气激发．ｘ分量与大气的相关性要强于ｙ分量，而且更为稳定，主要表现为平均时间尺度约为２７天的波动，大气对这个波动的贡献可达７０％．     

Optimizing point-source parameters for scanning satellite surveys

We describe a method for deriving the position and flux of point and compact sources observed by a scanning survey mission. Results from data simulated to test our method are presented, which demonstrate that at least a 10-fold improvement is achievable over that of extracting the image parameters, position and flux, from the equivalent data in the form of pixel maps. Our method achieves this improvement by analysing the original scan data and performing a combined, iterative solution for the image parameters. This approach allows for a full and detailed account of the point-spread function (PSF), or beam profile, of the instrument. Additionally, the positional information from different frequency channels may be combined to provide the flux-detection accuracy at each frequency for the same sky position. Ultimately, a final check and correction of the geometric calibration of the instrument may also be included. The Planck mission was used as the basis for our simulations, but our method will be beneficial for most scanning satellite missions, especially those with non-circularly symmetric PSFs.