华南前汛期降水异常及其环流特征分析

利用国家气候中心整编的中国160站的月平均降水资料和美国NCEP/NCAR的再分析资料,分析华南前汛期降水的异常及其环流特征。文中取“九五”重中之重项目执行组指出的华南地区的16站来代表华南地区,侧重分析了华南前汛期降水异常的年际、年代际变化特征及华南前汛期多、少雨年同期的环流特征。研究发现：华南地区降水的季节分布呈现双峰型,两个峰值分别在6月和8月。华南前汛期近50年的总的降水趋势变化不明显。1950年代前期和1960年代中期—1980年代中为相对多雨期,而1950年代中期—1960年代中期以及1980年代中期—1990年代初为相对少雨期,1990年代为正常波动期。华南前汛期降水存在3 a、5 a、7 a、14 a的周期。在分析华南前汛期多、少雨年大气环流场的特征时发现：华南前汛期多雨年时南亚高压和副高都偏弱,华南地区低层的水汽通量辐合加强,而且低空辐合,高空辐散,气流上升运动加强,容易形成降水;而少雨年的情况恰恰相反。     

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。     

Classification of stellar spectra with SVM based on within-class scatter and between-class scatter

Support Vector Machine (SVM) is a popular data mining technique, and it has been widely applied in astronomical tasks, especially in stellar spectra classification. Since SVM doesn’t take the data distribution into consideration, and therefore, its classification efficiencies can’t be greatly improved. Meanwhile, SVM ignores the internal information of the training dataset, such as the within-class structure and between-class structure. In view of this, we propose a new classification algorithm-SVM based on Within-Class Scatter and Between-Class Scatter (WBS-SVM) in this paper. WBS-SVM tries to find an optimal hyperplane to separate two classes. The difference is that it incorporates minimum within-class scatter and maximum between-class scatter in Linear Discriminant Analysis (LDA) into SVM. These two scatters represent the distributions of the training dataset, and the optimization of WBS-SVM ensures the samples in the same class are as close as possible and the samples in different classes are as far as possible. Experiments on the K-, F-, G-type stellar spectra from Sloan Digital Sky Survey (SDSS), Data Release 8 show that our proposed WBS-SVM can greatly improve the classification accuracies.     

Nonlinear analytic solution for perturbed relative motion using differential equinoctial elements

This paper develops a nonlinear analytic solution for satellite relative motion in J₂-perturbed elliptic orbits by using the geometric method that can avoid directly solving the complex differential equations. The differential equinoctial elements (DEEs) are used to remove any singularities for zero-eccentricity or zero-inclination orbits. Based on the relationship between the relative states and the DEEs, state transition tensors (STTs) for transforming the osculating DEEs and propagating the mean DEEs have been derived. The formulation of these STTs has been split into a set of vector and matrix operations, which avoids directly expanding the complex second-order terms, and thus, the obtained STTs could be easy-to-understand and easy-to-code. Numerical results show that the proposed nonlinear solution is valid for zero-eccentricity and zero-inclination reference orbit and is more accurate than the previous linear or nonlinear methods for the long-term prediction of satellite relative motion.     

基于DBBC＋Mark5B记录系统的脉冲星观测

2009年11月,云南天文台射电天文研究团组采用40m射电望远镜以及基于DBBC（Digital Base Band Conveter）和Mark5B的VLBI记录系统对PSRJ08354510和PSRJ0332＋5434进行了观测。观测选用S波段右旋圆极化信号,起始频率为2206．99MHz,总带宽为32MHz。对数据进行相干消色散和平均后,得到PSRJ0332＋5434的单脉冲图像和两颗脉冲星的平均脉冲轮廓。由平均轮廓的展宽随时间的变化关系,对脉冲星的视周期作了一定修正后,得到信噪比更高的平均轮廓图。最后对轮廓的信噪比随时间的变化作了初步分析,由此可了解整个系统在观测时的稳定性。     

2007年西北太平洋热带气旋定位和预报精度评定

依据<台风业务和服务规定>分析2007年TC业务定位和业务预报精度,结果表明:各方法的平均定位误差均小于25km,强度预报的24小时和48小时近中心最大风速平均误差为3～7m·s-1和5～11m·s-1,均与往年相当;综合预报的24小时和48小时路径平均距离误差分别为129.8km和215.0km.虽然路径数值预报的能力仍然不能与综合预报相比,但是多模式集成方法相对于综合预报有正技巧,说明这类方法可能成为改善路径预报的途径之一.强度预报的主要参考仍然是统计类预报方法.     

太阳中微子问题

文中从中微子物理学、太阳中微子的探测、标准太阳模型的建立等方面对太阳中微子问题的提出进行了回顾。各为太阳中微子探测器测量结果不同程度的偏低，以及不同类探测器测量结果之间的矛盾，使得人们对太阳中微子的研究表现出浓厚的兴趣。对太阳中微子问题可从粒子物理和天体物理两个方面进行研究。文中分别对这两个研究领域中提取的企图解决太阳中微子问题的模型作了简要评述。     

Solving the G-dwarf problem with a three-component model of the chemical evolution of the Galaxy

A three-component chemical evolution model of the Galaxy is presented, which we believe will cast a new light on the G-dwarf problem. The model is based on a scenario of the Galaxy consisting of three major evolutionary phases: halo, thick disk and thin disk, separated by two short interludes of rapid collapse. The evolution of different stellar populations are treated separately, the combination of which yields an overall metallicity distribution function for the solar neighbourhood. We tested three different models using the same set of basic equations: the “prompt initial enrichment” (PIE) model, the “proportional yield” (PPY) model and the “collapse” (CLP) model. Best-fit parameters are derived. The results show that the different populations have remarkably different IMFs, while mass exchange has only minimally affected the chemical evolution in the solar vicinity, so that the solar vicinity can be regarded as a closed system, at least in the late stage of the Galactic evolution.     

云南强震和月相、白赤交角的关系

考察本世纪云南强烈地震与月相和白赤交角的关系。结果表明云南强震与月相的关系呈区带性的相关。中甸丽江带的强震大多发生在望;巧家宜良带多发生于朔和望;而大关马边带的强震则完全不发生在朔和望。另一结果显示：本世纪云南１３次７级以上的强烈地震中１１次发生在月球白赤交角的极值年及其前后２ａ（年）中,尤以勐海、耿马、峨山特别明显。通海峨山强震则发生在白赤交角最大值处     

Feedback of Active Galactic Nuclei in Seyfert 2 Galaxies

It is well accepted that feedback from active galactic nuclei (AGNs) plays an important role in the coevolution of the supermassive black hole (SMBH) and its host galaxy,but the concrete mechanism of feedback remains unclear.A considerable body of evidence suggests that AGN feedback suppresses star formation in the host galaxy.We assemble a sample of Seyfert 2 galaxies with recent observational data of compact nuclear starbursts and estimate the gas surface density as a function of column density to illuminate the relation between feedback and AGN properties.Although there are some uncertainties,our data still imply the deviation from the star formation law (Kennicutt-Schmidt law).Further,they indicate that:(1) Feedback correlates with the Eddington ratio,rather than with the mass of SMBH,as a result of decreasing star formation efficiency.(2) The SMBH and the torus are probably undergoing coevolution.Conclusions presented here can be refined through future high resolution CO or HCN observations.