云南天文台高分辨太阳光球CCD图象系统

介绍了配置在云南天文台太阳精细结构望远镜的高分辨光球ＣＣＤ图象系统的总体性能、硬件配置、附加光学系统和软件。给出了它的技术检测和试用结果。最后提出了若干改进和完善的考虑,以及对有关观测和研究方面的一些预期和展望。     

银河系卫星星系研究进展

对银河系内卫星星系进行全面的"人口普查"具有重要的意义。目前已经发现了二十几个卫星星系,其光度范围分布很广,最暗的矮星系比球状星体还暗。叙述了卫星星系的光度分布、空间分布和动力学性质。总结了观测和理论研究进展,并讨论了星流和伽玛射线在研究银河系结构和暗物质性质方面的贡献。表明了卫星星系的统计分布能用来很好地限制冷暗物质理论和星系形成的相关物理过程,同时指出当前研究的局限性和可能的发展方向。     

ICRF的现状分析及未来的发展

该文简要回顾了ICRF的发展历史和现状。介绍了天球参考架之间的连接和综合。根据目前ICRF的特点及研究现状和进展,以ICRF的精度、数据采集的精度、源结构的分析及ICRF定义源的选取标准等方面深入分析了当前ICRF存在的缺陷,并结合当前的各种软硬件条件分析了ICRF的改进趋势,对未来的ICRF建立和维持作了展望。     

日震学研究进展

日震学旨在通过对太阳震荡的观测和分析来研究太阳内部的结构和动力学。回顾了日震学产生和发展的历史过程,简单介绍了太阳震荡的基本性质和部分观测仪器,综述了全球日震学与局部日震学的研究方法和近年来取得的部分重要进展,指出了日震学研究是理解太阳内部结构不可替代的工具,其研究成果具有极其重要的意义。     

绕月探测工程地面接收站通用解调处理机性能测试

介绍了绕月探测工程数据接收地面站使用的通用解调处理机的基本组成和工作原理;讨论了针对误码率、极化合成、帧同步和滑步容错等指标要求的测试原理和方法,并对其测试结果进行了分析。为卫星通信的基带设备的测试提供了参考。     

逐日追食——TWAN全方位追逐2010日全食

TWAN——“夜空下的世界”是2009国际天文年的一个特别项目。TWAN将世界上著名的摄影师、天文学家和组织机构凝聚在一起形成了一个新的国际团队。2009年TWAN成功地举行了一系列摄影展览和讲座。这些在恒星、行星和天象映衬下的,世界风景名胜的照片和视频深深震撼了各地的民众。     

嫦娥二号任务地面应用系统实时业务仿真关键技术研究

通过分析探月工程二期嫦娥二号(Chang’E-2,CE-2)任务地面应用系统的结构和功能,提出了实时业务系统的仿真模型。根据实时业务的功能特点进行了关键技术分析及仿真系统设计和实现。最后针对关键技术问题进行了仿真试验及结果分析,提出了解决问题的思路和方法。论文为嫦娥二号任务地面应用系统数据仿真系统的建立提供了基础。     

GPS卫星的激光测距和应用研究

简述了SLR和GPS跟踪技术的发展概况。详细介绍了近几年来对GPS－35、36卫星的激光测距进展和应用研究的情况。给出了残差分析的初步结果,并指出了目前GPS卫星的稀少的激光测距资料对卫星精密定轨和站坐标的解算是有价值的。同时,也简单地评述了GPS卫星的微波和激光跟踪技术各自的优势和弱点．建议联合利用GPS-35、36卫星的SLR和GPS观测资料来开展有关的应用研究。最后,对今后的应用研究工作提出了建议．     

罗兰C自主TOC同步的研究

研究了罗兰C自主实现TOC同步的原理。根据TOC的特点 ,分析了罗兰C自主TOC同步的基本要求。定义了TOC信息的概念 ,提出了一种新的信息类型和相应的通信规约。分析了GRI脉冲序列与参考脉冲 ,以及调制码组与罗兰C脉冲组的时间关系。最后详细研究了在连续传输 (TOC信息和DGNSS交替 )方式下TOC同步的原理和方法。     

一种基于DSP和FPGA的低频时码接收机设计

介绍了一种基于数字信号处理器(DSP)和现场可编程门阵列(FPGA)的低频时码接收机的硬件组成,描述了该接收机系统实现时间同步的方法,阐述了DSP和FP-GA的软件设计,给出了测试和仿真结果。该设计方案具有精度高、可靠性强、扩展性好等优点。     

Long-Term Stability Analysis of Quasi Integrable Degenerate Systems Through the Spectral Formulation of the Nekhoroshev Theorem

We describe a numerical application of the Nekhoroshev theorem to investigate the long-term stability of quasi-integrable systems. We extend the results of a previous paper to a class of degenerate systems, which are typical in celestial mechanics.     

Numerical model of the influence function of deformable mirrors based on Bessel Fourier orthogonal functions

A numerical model is presented to simulate the influence function of deformable mirror actuators. The numerical model is formed by Bessel Fourier orthogonal functions, which are constituted of Bessel orthogonal functions and a Fourier basis. A detailed comparison is presented between the new Bessel Fourier model, the Zernike model, the Gaussian influence function and the modified Gaussian influence function. Numerical experiments indicate that the new numerical model is easy to use and more accurate compared with other numerical models. The new numerical model can be used for describing deformable mirror performances and numerical simulations of adaptive optics systems.     

Using the transition to action variables of the newtonian problem in the numerical solution of the N-body problem

We propose an approach for overcoming the problem of close encounters in collisional systems, globular and open star clusters. As is well known, the numerical integration step in such systems, for example, during the formation of close binary stars, begins to fragment and the rate of calculations goes down to a complete stop. We show that using the perturbation theory in the proposed approach, one can isolate the singularity and to increase considerably the integration step without losing the physical effects that affect significantly the evolution of star clusters.     

On the numerical evaluation of theJ-integrals

This is a third paper dealing with the numerical evaluation of the light changes exhibited by close binary systems; for previous communications, Lanzano, 1976a, b.TheJ-integrals which were introduced by Kopal for the purpose of this numerical evaluation can be expanded in terms of the Appell hypergeometric series of the first kind. This relationship has been instrumental in establishing a number of recursion formulae for theJ-integrals applicable to the case of an annular eclipse. It was found that some recursion formulae hold both for the case of a partial and annular eclipse.The appropriate use of these recursion formulae should facilitate any numerical computation for eclipsing binaries.     

辛算法在动力天文中的应用（Ⅲ）

文［１］和文［２］从哈密顿系统的整体结构保持一角度阐明了辛算法［３－６］的主要功能，本文将从定量的角度进一步表明辛算法的另一独特优点－可以控制天体运动沿迹误差的快速增长，并对可分离哈密顿系统的显式辛差分格式稍加改进，推广应用到一般动力系统，该系统含有小耗散项或小的不可分离项，计算结果表明，效果极佳，因此，辛算法与传统的数值解法相比，确有很多优点。     

Hyperbolic character of the angular moment equations of radiative transfer and numerical methods

We study the mathematical character of the angular moment equations of radiative transfer in spherical symmetry and conclude that the system is hyperbolic for general forms of the closure relation found in the literature. Hyperbolicity and causality preservation lead to mathematical conditions allowing us to establish a useful characterization of the closure relations. We apply numerical methods specifically designed to solve hyperbolic systems of conservation laws (the so-called Godunov-type methods) to calculate numerical solutions of the radiation transport equations in a static background. The feasibility of the method in all regimes, from diffusion to free-streaming, is demonstrated by a number of numerical tests, and the effect of the choice of the closure relation on the results is discussed.     

等级三星系统的运动学研究

统计分析表明,在目前的观测精度(Imas)下,由于三体效应大多数等级三星系统已不能用经典的双二体运动学模型来描述;即使对于应用需求而言,该模型也不再适用于描述三体视效应较强的等级三星系统.因为在实用星表参考架中不宜采用数据量较大的数值历表来描述子星的运动,所以有必要针对等级三星系统建立尽可能简单实用的运动学模型.借助已有的观测资料和拟合研究结果,给出了6个等级三星系统的质量参数和初始条件,进而根据实用需求讨论了这些系统的运动学描述问题.     

Computation of the elements of close eclipsing systems in the frequency-domain

The aim of the present paper will be to generalize the methods for computation of the elements of eclipsing binary systems in the frequency-domain, summarized in our recent Paper I (Kopal, 1981), to the case ofclose systems, in which photometric proximity effects become conspicuous and must be taken into account before the methods previously outlined in Paper I become directly applicable.Following a brief introduction to the subject given in Section 1, Section 2 summarizes (and comments upon) the difficulties previously encountered in separation of the photometric proximity and eclipse effects. In Section 3 we develop an alternative new approach to the problem by modulation of the light curves throughout the entire orbital cycle, intended to filter out proximity effects from the observed light changes and isolate those due to eclipses; while in Section 4 we shall present a numerical application of the new method to an analysis of the observed light changes of the eclipsing system W Ursae Maioris.In Section 5 we shall present a quantitative investigation of the photometric effects of distortion on the light changes of close eclipsing systems within eclipses-the most complicated part of the whole problem-with numerical application to the system of U Sagittae carried out in the concluding Section 6.Appendices 1–3 contain numerical data which should facilitate application of the methods developed and illustrated in Sections 3–4; while Appendix 4 will be reserved for a mathematical proof of certain expansions used in Section 5, which would have been too discursive for the main text.     

Recent developments of integrating the gravitational problem ofN-bodies

This paper discusses the formulation and the numerical integration of large systems of differential equations occurring in the gravitational problem ofn-bodies.Different forms of the pertinent differential equations of motion are presented, and various regularizing and smoothing transformations are compared. Details regarding the effectiveness and the efficiency of the Kustaanheimo-Stiefel and of other methods are discussed. In particular, a method is described in which some of the phase variables are treated in the regularized system and others in the ordinary system. This mixed method of numerical regularization offers some advantages.Several numerical integration techniques are compared. A high order Runge-Kutta method, Steffensen's method, and a finite difference method are investigated, especially with regard to their adaptability to regularization.The role of integrals and integral invariants is displayed in controlling the accuracy of the numerical integration.Numerical results are described with 5, 25 and 500 bodies participating. These examples compare the various integration techniques, several regularization methods and different logics in treating binaries.