螺线管磁定位技术初探

随着钻探工艺的不断发展,对井身轨迹的要求不断增加。一般依靠地磁定位的仪器已无法满足精度要求,于是研发出了多种近场磁导向系统,如MGT、RMRS和慧磁中靶仪等。以发射源种类为依据,可分为主动测量技术和被动测量技术。螺线管磁定位系统属于主动测量技术,它具有数据传输量小、耐温高等优点。目前国外已经商用化,而国内研究不多。本文简单介绍了螺线管测量的理论模型,着重阐述了室内实验和误差分析。实验共测量了144个点数据,总距离平均误差为4.9%,平面距离平均误差为5.6%,初步验证了螺线管磁定位系统的可行性。     

地震社会心理初探与政府的疏导防治对策

针对我国当前较具典型的几种地震社会心理，指出职能部门疏导、防治的工作重点，并从顺应国情、民情及国家经济体制改革的方向出发，提出相应的对策建议。     

我国对越南直接投资初探

本文从理论和实际的结合上，论述了我国开展对越直接投资的必要性和可能性。文中对投资机遇、边境贸易、对越经援等问题作了深入分析，并提出了对越投资的产业导向和区域战略。     

Irradiance observations of the 1–8 Å solar soft X-ray flux from goes

The solar 0.5–8 soft X-ray flux was monitored by the NOAA Geostationary Operational Environmental Satellites (GOES) from 1974 to the present, providing a continuous record over two solar activity cycles. Attempts have been made to determine a soft X-ray (SXR) background flux by subtracting out solar flares (using the daily lowest flux level). The SXR background flux represents the quiescent SXR flux from heated plasma in active regions, and reflects similar (intermediate-term) variability and periodicities (e.g. 155-day period) as the SXR or hard X-ray (HXR) flare rate, although it is determined in non-flaring time intervals. The SXR background flux peaks late in Solar Cycle 21 (2–3 years after the sunspot maximum), similar to the flare rate measured in SXR, HXR, or gamma rays, possibly due the increasing complexity of coronal magnetic structures in the decay phase of the solar cycle. The SXR background flux appears to be dominated by postflare emission from the dominant active regions, while the contributions from the quiet Sun are appreciable in the Solar Minimum only (A1-level). Comparisons with full-disk integrated images from YOHKOH suggest that the presence of coronal holes can decrease the quietest SXR irradiance level by an additional order of magnitude, but only in the rare case of absence of active regions.Presented at IAU Colloquium No. 143, The Sun as a Variable Star: Solar and Stellar Irradiance Variations, Boulder, CO, June 20–25, 1993     

山东省天气预报逐级指导技术研究

介绍了山东省天气预报逐级指导技术研究的技术方法和预报逐级指导业务系统；给出了常规要素、冰雹和暴雨预报对比试验的TS评分结果和研究结论。     

Spacecraft potential control aboard Equator-S as a test for Cluster-II

The payload of Equator-S was complemented by the potential control device (PCD) to stabilise the electric potential of the spacecraft with respect to the ambient plasma. Low potentials are essential for accurate measurements of the thermal plasma. The design of PCD is inherited from instruments for Geotail and Cluster and utilises liquid metal ion sources generating a beam of indium ions at several keV. The set-up of the instrument and its interaction with the plasma instruments on board is presented. When the instrument was switched on during commissioning, unexpectedly high ignition and operating voltages of some ion emitters were observed. An extensive investigation was initiated and the results, which lead to an improved design for Cluster-II, are summarised. The cause of the abnormal behaviour could be linked to surface contamination of some emitters, which will be monitored and cured by on-board procedures in future. The mission operations on Equator-S were not at all affected, because of the high redundancy built into the instrument so that a sufficient number of perfectly operating emitters were available and were turned on routinely throughout the mission. Observations of the effect of spacecraft potential control on the plasma remained limited to just one event on January 8, 1998, which is analysed in detail. It is concluded that the ion beam lead to the predicted improvement of the particle measurements even outside the low density regions of the magnetosphere where the effect of spacecraft potential control would have been much more pronounced, and that the similar instruments for the four Cluster-II spacecraft to be launched in 2000 will be very important to ensure accurate plasma data from this mission.     

高光谱图像滚动引导递归滤波与地物分类

高光谱图像类内光谱变化较大,"同物异谱"现象普遍存在。利用原始地物光谱特征进行分类精度较低而且分类结果图中存在"椒盐现象"。为了获得好的分类结果,必须充分利用高光谱图像的光谱信息和空间信息,减少类内的光谱变化,并扩大类别间的光谱差异。为此,提出一种滚动引导递归滤波的高光谱图像光谱—空间分类方法。首先,利用主成分分析对高光谱图像进行降维;然后,利用高斯滤波对输入图像进行模糊化,消除图像中的噪声和小尺度结构;接下来,将模糊化后的图像作为引导图像,对输入图像进行边缘保持递归滤波,输出结果作为新的引导图像,重复迭代这个过程直至大尺度边缘被恢复;最后,利用提取的特征波段和支持向量机对高光谱图像进行分类。在两个真实高光谱数据集上进行了分类实验,结果表明本文方法的分类精度优于其他的高光谱图像分类方法。在训练样本极少的情况下,本文方法也能获得较高的分类精度。     

浅析提升测绘质量建设的几点做法

结合作者多年从事测绘生产与管理实践经验,对如何抓好质量建设做了深入的分析与思考,从文化、制度、人员、管理和创新5个方面入手,阐述了质量理念、体制机制、业务能力、指导验收、创新方法在质量建设中的作用.     

盾构机自动导向系统坐标解算及实现效果分析

分析了日本演算工房盾构机自动导向系统,提出其坐标解算原理,并进行了实现效果分析。     

Europa's opposition surge in the near-infrared: interpreting disk-integrated observations by Cassini VIMS

Near-infrared observations of Europa's disk-integrated opposition surge by Cassini VIMS, first published in Fig. 4 of Brown et al. (2003, Icarus, 164, 461), have now been modeled with the commonly used Hapke photometric function. The VIMS data set emphasizes observations at 16 solar phase angles from 0.4° to 0.6°—the first time the <1° phase “heart” of Europa's opposition surge has been observed this well in the near-IR. This data set also provides a unique opportunity to examine how the surge is affected by changes in wavelength and albedo: at VIMS wavelengths of 0.91, 1.73, and 2.25 μm, the geometric albedo of Europa is 0.81, 0.33, and 0.18, respectively. Despite this factor-of-four albedo range, however, the slope of Europa's phase curve at <1° phase is similar at all three wavelengths (to within the error bars) and this common slope is similar to the phase coefficient seen in visible-light observations of Europa. The two components of the opposition surge—involving different models of the physical cause of the surge—are the Shadow Hiding Opposition Effect (SHOE) and the Coherent Backscatter Opposition Effect (CBOE). Because of sparse VIMS phase coverage, it is not possible to constrain all the surge parameters at once in a Hapke function that has both SHOE and CBOE; accordingly, we performed separate Hapke fits for SHOE-only and CBOE-only surges. At 2.25 μm, where VIMS data are somewhat noisy, both types of surges can mimic the slope of the VIMS phase curve at <1° phase. At 0.91 and 1.73 μm, however—where VIMS data are “cleaner”—CBOE does a noticeably poorer job than SHOE of matching the VIMS phase coefficient at <1° phase; in particular, the best CBOE fit insists on having a steeper phase-curve slope than the data. This discrepancy suggests that Europa's near-IR opposition surge cannot be explained by CBOE alone and must have a significant SHOE component, even at wavelengths where Europa is bright.