天文学英语新词自动提取系统

科技名词中文译名标准化和规范化工作是推动我国科技进步和科学知识传播的重要基础。新的科学概念和技术名词层出不穷,如何及时发现并确定新生术语的中文译名是一项普遍的社会需求。介绍了一套全新的天文学英语新词自动提取系统。该系统综合使用脚本过滤、术语识别、正则表达匹配等多种方法,能够自动追踪Ar Xiv论文数据库的更新,分析天文学论文的内容,生成推荐术语列表,从而将学科专家从繁重的科技新词收集整理工作中解放出来,把有限的精力集中到更能体现专业素养的新词审定工作当中。这个系统将为推动天文学等基础学科的新词收集,乃至学科标准化等工作发挥积极作用。     

人工影响天气用碘化银催化剂对区域环境影响的研究进展

中国自1958年以来开展人工影响天气作业。碘化银作为主要的催化剂,是否会对环境造成影响备受关注。分析了国内外使用碘化银开展人工增雨雪和人工防雹外场试验作业后降水、土壤和湖泊等的Ag+含量,尽管催化后Ag+含量会有不同程度的增加,尤其是地面燃烧炉催化和人工防雹作业,但降水和水库中的Ag+含量远低于饮用水标准。统计了我国外场人工影响天气作业的碘化银用量,结合降水和水库中Ag+浓度观测,认为我国人工影响天气使用的碘化银不会对水资源和环境造成影响。     

全球气候变化中的人类活动视角:社会经济情景的演变

社会经济情景的设定是全球气候变化研究的基础,也是气候变化影响评估的关键环节.本文回顾了社会经济情景的发展过程,阐述了共享社会经济路径的主要特点和最新发展趋势,介绍了区域社会经济情景的构建及在灾害风险领域中的应用,最后对共享社会经济路径的发展进行了展望.     

基于分段函数法计算湿球温度研究

核电厂冷却塔设计气象条件中,湿球温度是重要的设计气象参数之一。近年来,由于实行自动观测,相对湿度值由仪器自动测定,因此不少气象站已经停止了湿球温度的观测,这给电厂气象参数的分析计算造成了一定困难。为此,根据气压分布型特点和分段函数,提出利用干球温度和相对湿度来计算湿球温度的新方法,经河南省郑州、南阳和商丘3站的应用,效果良好。     

登陆华南热带气旋强度变化与大尺度环流的关系

应用UK再分析资料,采用合成分析方法,对比分析了登陆华南的登陆前迅速增强的TC（Rapid Intensifying TC,简称RITC）和迅速减弱的TC（Rapid FillingTC,简称RFTC）登陆前24h的大尺度环流背景特征。结果表明：从外流、入流强度和范围上看,RITC的低空入流和高空外流均明显强于RFTC,两类TC高空外流强度的差异比低空入流明显,RITC的次级环流径向范围大;从外流垂直伸展高度上看,RITC的平均外流主要集中在500hPa以上,而RFFC的平均外流比较分散,向下伸展到850hPa;从高空流场配置看,RITC上空除西北象限外均有较强外流,而RVrC仅在东北象限有较强外流,相应的RITC和RVrC的高空辐散在范围和强度上均有明显的差异,其中RITC的高空辐散明显强于RFTC;强烈的西南季风水汽输送是登陆华南的TC登陆前突然加强的先兆条件,RITC的对流活动明显比RFTc活跃;RITC的纬向风垂直切变比RFTC小,有利于RITC的强度增强。     

40m天线面板调试与精度分析

总结了40m天线面板安装调试及检测的过程，分析了反映望远镜面板指标的吨性能检测结果。结果表明天线面板精度优于原设计要求。     

利用小波变换进行遥感多光谱图像融合的算法及实现

在分析了小波变换的分解与重建方法后,提出了一种基于区域的图像增强算法。先提取出源图的边缘,以图像的边缘为参考,围绕边缘建立融合窗口,然后结合区域内的图像信息,应用基于窗口的融合规则进行融合处理。实验结果显示,融合后的图像综合了3幅源图像的不同特征,处理后的图像变得容易识别了。表明该方法保持了尽可能多的原始信息,算法简单,稳定性好,适合于多光谱遥感图像识别、医学成像等领域。     

Brew平台上应用程序中断和恢复的处理

介绍了手机软件开发的应用BREW平台。主要阐述了运用于手持设备的应用程序在开发时所做的中断和恢复处理。     

A New Method of Identifying 3D Null Points in Solar Vector Magnetic Fields

Employing the Poincare index of isolated null-points in a vector field, we worked out a mathematical method of searching for 3D null-points in coronal magnetic fields. After introducing the relevant differential topology, we test the method by using the analytical model of Brown & Priest. The location of null-point identified by our method coincides precisely with the analytical solution. Finally we apply the method to the 3D coronal magnetic fields reconstructed from an observed MDI magnetogram of a super-active region (NOAA 10488). We find that the 3D null-point seems to be a key element in the magnetic topology associated with flare occurrence.     

Unusual spectral absorption observed in the 16 August 1989 limb flare

A relative complete set of He I 10830 Å profiles and their coincident slit-jaw Hα images of the large limb flare (2N/X20) of 16 August 1989 were observed by the solar spectrograph at Purple Mountain Observatory. In addition to the unusually broadened spectral profiles observed in the impulsive phase, more than half of the observed He I 10830 Å profiles are characterized by central reversals, which were detected not only in the impulsive phase but also in the late decaying phase. The central-reversed profiles may exist at different heights, ranging from the solar limb to (3–4) × 10⁴ km above. The absorption varies with time and position, with a typical lifetime and size of several minutes and 5–6 arc sec, respectively. Depths of the absorption profiles also change clearly. The absorptions are usually deeper at the loop footpoint near the solar limb and shallower at loop-top. However, the most unusual feature is that all the line-center wavelengths of them show no shift relative to that of the quiet chromosphere near the limb, implying the apparent velocities are zero while the associated emission profiles have different apparent velocities. Theoretical simulations demonstrate that the Doppler widths of the absorptions are in the range of (0.35–0.5)Å and increase with height, and the source functions are (0.11–0.3) times the disk center intensity. However, the absorptions have a relative large range of optical thickness (0.1–1.3) in the I ₃ component of the He I 10830 Å triplet. We have not observed such absorption in other limb flares, including the SB/X2.9 flare of 17 August 1989 that occurred in the same active region as the studied one (NOAA 5629). Our studies show that the absorption could not result from he scattering by the telluric atmosphere or from normal chromospheric absorption. This unique phenomenon may be related to extra intense X-ray flux and caused by diffuse and non uniform materials dissociated from the flare instead of self-absorption of the flare.