半实物仿真中三轴转台误差分析

介绍了半实物仿真中三轴转台的设备参数修正方法,根据此结果对影响转台精度的频率特性进行测试,并从理论上给出转台框架误差的分析结果。     

Element Abundances in X-ray Emitting Plasmas in Stars

Studies of element abundances in stars are of fundamental interest for their impact in a wide astrophysical context, from our understanding of galactic chemistry and its evolution, to their effect on models of stellar interiors, to the influence of the composition of material in young stellar environments on the planet formation process. We review recent results of studies of abundance properties of X-ray emitting plasmas in stars, ranging from the corona of the Sun and other solar-like stars, to pre-main sequence low-mass stars, and to early-type stars. We discuss the status of our understanding of abundance patterns in stellar X-ray plasmas, and recent advances made possible by accurate diagnostics now accessible thanks to the high resolution X-ray spectroscopy with Chandra and XMM-Newton.     

中国民航空管步入全面英语管制时代

3月5日起,中国民航空管系统实施无线电通信指挥的管制人员必须具备国际民航组织管制英语四级及以上水平,开始全面推行使用英语进行无线电通话工作。     

安全路由器关键技术探讨

路由器是网络架构巾的重要部件。在网络安全越来越受到重视的今天,为了提高所传输数据的安全性,安全路由器应运而生。文中介绍了安全路由器的解决方案,探讨了应用于安全路由器上的防火墙、VPN、IDS、加密、认证等几种主要的路由器关键技术。     

Be stars in young clusters in the Magellanic Clouds

A substantial fraction (typically 10%) of Galactic B stars consists of Be stars. While Galactic Be stars have been fairly well investigated, very little is known about the Be star content of the Magellanic Clouds (MCs). We present a refined method of Be star identification by CCD photometry and apply it to four young clusters and associations in the MCs. We find NGC 330 in the SMC to be exceptionally rich in Be stars, while the fraction is clearly lower in the similarly aged LMC clusters NGC 2004 and NGC 1818. NGC 2044, a very young region in the LMC, contains almost no Be stars. Among very early-type B stars in the investigated MC clusters we find the largest number of Be stars, while in the Milky Way this is shifted to somewhat later types. In the LMC, there may be a second frequency peak around B6.Based on observations obtained at the 2.2m MPIA telescope at ESO, La Silla, Chile, partly on time granted by the MPIA, Heidelberg.     

Mass flow in interacting binaries observed in the ultraviolet

Recent satellite observations of close binary systems show that practically all binaries exhibit evidence of mass flow and that, where the observations are sufficiently detailed, a fraction of the matter flowing out of the mass-losing component is accreted by the companion and the remainder is lost from the binary system. The mass flow is not conservative. During the phase of dynamic mass flow, the companion star becomes immersed in optically-thick plasma and the physical properties of that star elude close scrutiny.     

Mass flow in interacting binaries observed in the ultraviolet

Recent satellite observations of close binary systems show that practically all binaries exhibit evidence of mass flow and that, where the observations are sufficiently detailed, a fraction of the matter flowing out of the mass-losing component is accreted by the companion and the remainder is lost from the binary system. The mass flow is not conservative. During the phase of dynamic mass flow, the companion star becomes immersed in optically-thick plasma and the physical properties of that star elude close scrutiny.     

风洞试验绳牵引并联支撑技术研究进展

新型飞行器的研制越发强调先进的飞行性能,这对风洞试验模型支撑技术提出了高的要求,为扩展风洞试验的能力,迫切需要研究新型的智能支撑技术。绳牵引并联支撑是基于机器人技术的一种新型机构,具有刚度较大,动态性能良好等优点,为风洞试验提供了一种新的手段。首先,全面论述了绳系支撑在风洞试验中的应用,并给出动态分析;进一步根据绳牵引并联支撑技术的特点,将其分为可实现受迫运动的冗余约束支撑,以及可实现受迫+自由运动的欠约束支撑;其次,重点阐述了冗余约束与欠约束两类支撑系统的若干关键技术问题及其研究进展;最后,指出绳牵引并联支撑技术的发展方向是具有可重构性和智能化。可为绳牵引并联支撑技术在风洞试验中的工程应用提供一定的理论指导与技术支持。     

茶在江南

茶,国饮也。发于神农,闻于周公,兴于唐朝,盛于宋代。中华茶文化糅合了儒、道、释诸家思想,涵盖了选茶、蓄水、煮茶、茶具、环境、情趣等饮茶的全过程,是中华传统文化中的一朵奇葩,芬芳而甘醇。古人认为茶有十德:以茶散郁气,以茶驱睡气,以茶养生气,以茶除病气,以茶利礼仁,以茶表敬意,以茶尝滋味,以茶养身体,以茶可行道,以茶可雅志。     

从科学管理到道本管理

目前这本书是我在山东教育台十四集电视节目《道本管理——让心灵回家》的文字版,比起音像版来,这个文字版又增加和补充了一些全新的内容。这本书的主题和内容是我自1983年学习西方管理开始,经历了近三十年的实践、研究、学习和思考的历程之后的心得,是在对西方管理的崇尚和实践遭遇瓶颈之后的一次对管理思想和实践的突破,是对许多企业管理问题的重新思考与定位。上个世纪九十年代,在熟悉使用西方的管理方法之后,在实践中为了解决企业中的问题,更是把这套管理模式中的制度化、标准化、程序化做到了极致,以为管理中所有的问题都可以被囊括,都     

Recent Advances in Understanding Particle Acceleration Processes in Solar Flares

We review basic theoretical concepts in particle acceleration, with particular emphasis on processes likely to occur in regions of magnetic reconnection. Several new developments are discussed, including detailed studies of reconnection in three-dimensional magnetic field configurations (e.g., current sheets, collapsing traps, separatrix regions) and stochastic acceleration in a turbulent environment. Fluid, test-particle, and particle-in-cell approaches are used and results compared. While these studies show considerable promise in accounting for the various observational manifestations of solar flares, they are limited by a number of factors, mostly relating to available computational power. Not the least of these issues is the need to explicitly incorporate the electrodynamic feedback of the accelerated particles themselves on the environment in which they are accelerated. A brief prognosis for future advancement is offered.     

Protons in flares

This work addresses the role of non-thermal protons as a means of transporting energy in stellar atmospheres. The most dramatic transient visible phenomena are flares, the best studied of which are from the Sun. It is believed that energetic particles take a fundamental part in flare development, but it is controversial as to whether protons or electrons play the dominant role. This review is aimed at helping resolve the controversy. We start by outlining acceleration mechanisms for energetic particles, on the premise that the acceleration site is in the corona. The propagation of a proton beam through the atmosphere is discussed, together with the radiation signatures it would produce. Chromospheric evaporation is expected as the beam reaches the dense part of the atmosphere. Direct observational evidence for energetic protons is reviewed, from gamma-ray production involving energies >30 MeV to H polarization, which is significant at energies 100 keV. Proton beams can be detected in the corona via slowly-drifting type III bursts, while they can be directly sampled by spacecraft and, at energies >1 GeV, by detectors on the Earth. A number of key flare observations and energy arguments are debated from the viewpoint of protons versus electrons. The conclusion is that primary non-thermal protons are much more important, in terms of total energy, than non-thermal electrons in flares, and that the bulk of the energetic electrons are secondary.     

机器学习在湍流模型构建中的应用进展

借助于高性能计算机和数据共享平台的发展,研究者可以获取大量的高分辨率湍流计算数据。近年来,随着深度神经网络等人工智能技术的发展,数据驱动的机器学习方法也开始应用于湍流模型中不确定度的量化以及模型的改进和构建中。湍流大数据与人工智能相结合是湍流研究的一个新领域。研究者在取得一定成果的同时也面临着诸多困难和挑战,例如模型的泛化能力和鲁棒性等。模型构建过程包含了数据处理、特征选择以及模型框架的选取与优化等诸多方面,这些方面在不同程度上影响模型的性能。本文从机器学习在湍流建模过程中的实现方法和模型的不同作用两方面分析总结了目前主要的研究工作进展,并对这类问题面临的挑战和未来的研究展望进行了阐述。     

Research on uncertainty in measurement assisted alignment in aircraft assembly

Operations in assembling and joining large size aircraft components are changed to novel digital and flexible ways by digital measurement assisted alignment.Positions and orientations（P＆O）of aligned components are critical characters which assure geometrical positions and relationships of those components.Therefore,evaluating the P＆O of a component is considered necessary and critical for ensuring accuracy in aircraft assembly.Uncertainty of position and orientation（U-P＆O）,as a part of the evaluating result of P＆O,needs to be given for ensuring the integrity and credibility of the result;furthermore,U-P＆O is necessary for error tracing and quality evaluating of measurement assisted aircraft assembly.However,current research mainly focuses on the process integration of measurement with assembly,and usually ignores the uncertainty of measured result and its influence on quality evaluation.This paper focuses on the expression,analysis,and application of U-P＆O in measurement assisted alignment.The geometrical and algebraical connotations of U-P＆O are presented.Then,an analytical algorithm for evaluating the multi-dimensional U-P＆O is given,and the effect factors and characteristics of U-P＆O are discussed.Finally,U-P＆O is used to evaluate alignment in aircraft assembly for quality evaluating and improving.Cases are introduced with the methodology.     

纳米压痕实验微米级深度硬度下降现象的研究(英文)

本文针对均匀材料微米级压痕深度,分析接触深度、接触面积、载荷以及加载时间几种因素对实验数据的影响,结合有限元数值模拟,说明压头几何缺陷、接触深度与接触面积的处理并不是造成微米级压痕硬度随压深增大而下降的主要原因,最可能的原因是材料的蠕变特性。进行了不同最大压深实验显示连续刚度法(CSM)将强化蠕变特性对硬度曲线的影响,证明造成该现象的重要原因是纳米压痕实验的实验方法问题。     

Astrophysics in 2006

The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the Universe) and others of which there are always many, like meteors and molecules, black holes and binaries.     

微波测量中电缆线变化的校正方法

根据三天线法的原理,提出了用三电缆线法来校正信号传输中由于电缆线的移动、弯曲或老化引起的电缆线传输特性的变化.该方法将三条电缆线两两组合成三对,进行三次连续的测量,从而得出电缆线的传输特性和校正因子,对测得的信号进行校正.该方法对传输信号而非反射信号的测量,克服了电缆线损耗引起的对交换反射计的使用限制.     

超燃冲压发动机再生冷却U型通道的热传导模型研究

本文主要对超燃冲压发动机再生冷却通道进行了设计和改良。首先提出U型冷却通道这种往返式流道的通道结构,并针对传统的同向流道和U型通道分别进行了一维程序建模,对比了两种通道的优劣。并针对U型通道进行了不同高宽比对肋间传热影响的讨论和改变通道截面积以提升通道整体冷却效果的研究。研究表明：U型通道能较明显的降低燃烧室壁面的局部高温,使得整体温度分布更加均匀;适当增加高宽比,可增加肋间壁面的传热,使通道两侧温度差拉低;适当减小高宽比,可增加底壁面的传热,使局部燃烧室壁温降低;渐变通道截面积的设计方案,对解决通道出口区域燃烧室壁温过高,起到了明显的改善作用。     

Nucleosynthesis in Supernovae

We present the status and open problems of nucleosynthesis in supernova explosions of both types, responsible for the production of the intermediate mass, Fe-group and heavier elements (with the exception of the main s-process). Constraints from observations can be provided through individual supernovae (SNe) or their remnants (e.g. via spectra and gamma-rays of decaying unstable isotopes) and through surface abundances of stars which witness the composition of the interstellar gas at their formation. With a changing fraction of elements heavier than He in these stars (known as metallicity) the evolution of the nucleosynthesis in galaxies over time can be determined. A complementary way, related to gamma-rays from radioactive decays, is the observation of positrons released in \(\beta^{+}\)-decays, as e.g. from \(^{26}\mbox{Al}\), \(^{44}\mbox{Ti}\), \(^{56,57}\mbox{Ni}\) and possibly further isotopes of their decay chains (in competition with the production of \(e^{+}e^{-}\) pairs in acceleration shocks from SN remnants, pulsars, magnetars or even of particle physics origin). We discuss (a) the role of the core-collapse supernova explosion mechanism for the composition of intermediate mass, Fe-group (and heavier?) ejecta, (b) the transition from neutron stars to black holes as the final result of the collapse of massive stars, and the relation of the latter to supernovae, faint supernovae, and gamma-ray bursts/hypernovae, (c) Type Ia supernovae and their nucleosynthesis (e.g. addressing the \(^{55}\mbox{Mn}\) puzzle), plus (d) further constraints from galactic evolution, \(\gamma\)-ray and positron observations. This is complemented by the role of rare magneto-rotational supernovae (related to magnetars) in comparison with the nucleosynthesis of compact binary mergers, especially with respect to forming the heaviest r-process elements in galactic evolution.