第44届巴黎航展观感

前不久,巴黎成功地举办了第44届航展。本文简要介绍了这届航届的举办情况,以及参加这届航展的体会和感受。     

信息与动态

301所举办第42届世界标准日活动2011年10月14日,301所举办第42届世界标准日庆祝活动。301所第42届世界标准日活动围绕第42届世界标准日口号"世界标准树立全球信心"进行主题发言。发言阐明了标准的重要作用,并阐述了标准化工作者的责任和使命,     

第四届国际实验流体力学会议通知

国际实验流体力学会议（International Conference on Experimental Fluid Mechanics，ICEFM）是庄逢甘院士等人发起、由中国主导创办的一项重要的国际会议。会议从1991年开始每隔3年举办一次，连续举办了3届。第一届会议于1991年6月在中国成都召开，第二届于1994年7月在意大利都灵召开，第三届于1997年6月在莫斯科Korolev 地区举行。非常遗憾的是，由于会议的组织和交接工作出现了问题，原定于2000年在美国举行的第四届会议未能如期举办，致使该项重要会议停办至今。     

航空新闻

第46届巴黎国际航空航天展开幕为期7天的第46届巴黎国际航空航天博览会6月13日在法国首都巴黎东北郊的布尔歇机场隆重举行。来自41个国家和地区的1916家世界航空航天工业巨头和中小企业代表、238架飞机参加了展览,有近百个国家和地区的上万名专业人士出席展览。中国派出了包括中国一航在内的四家集团公司以庞大阵容在本次航展亮相。在本届巴黎航展上,中国航空航天展品备受瞩目。第6届中国航展招商团赴巴黎航展招商成果喜人赴第46届巴黎航展招商的第6届中国(珠海)航展招商团圆满完成招商任务,满载而归。在为期7天的本届巴黎航展上,第6届中国(…     

42届巴黎航展现场实录

Pictures From ParisAir Show’9 742届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录42届巴黎航展现场实录vv42届巴黎航展现场实录     

关于和谐机场建设问题的思考

党的十六届六中全会作出了《中共中央关于构建社会主义和谐社会若干重大问题的决定》;民航总局党委制定下发了《关于贯彻党的十六届六中全会精神建设和谐民航的意     

“第六届《飞行器测控学报》编委会第一次工作会议”情况简报

第五届《飞行器测控学报》（以下简称《学报》）编委会自2004年6月成立以来，认真履行职责，圆满完成了任期内的各项工作。根据编委会组织制度，经各有关单位的积极推荐，换届成立了以《学报》主管单位北京跟踪与通信技术研究所钱卫平所长为主任委员的第六届《学报》编委会。为回顾第五届《学报》编委会的工作，总结经验，发现不足，讨论、确定第六届《学报》编委会的工作规划、     

航空先进制造技术展望报告及第六届工艺专业委员会在京举行

中国航空学会工艺专业委员会于2000年4月24日～26日在北京625所召开了“航空先进制造技术展望报告及第六届工艺专业委员会全体委员会”。参加会议的50余名代表分别来自航空、航天的厂、所、院校和杂志社、机关等32个单位。会议由工艺专业委员会副主任刘善国、黄麟綦共同主持。会上 ,第五届中国航空学会工艺专业委员会主任胡建国研究员作了第五届工艺专业委员会工作总结报告。中国航空学会组织部王树青部长宣读了聘任第六届工艺专业委员会委员文件 ,宣告第六届中国航空学会工艺专业委员会成立。接着会议进入技术报告议程 ,请特邀专家学者作“航空先进制造技术展望”学术报告。     

中国宇航学会第三届材料工艺专业委员会成立大会暨技术交流会胜利召开

中国宇航学会第三届材料工艺专业委员会成立大会暨技术交流会胜利召开１９９４年１０月２０日至２２日，在中国航天工业总公司第一研究院长征宾馆召开了中国宇航学会第三届材料工艺专业委员会成立大会暨技术交流会，出席会议的有第二届和第三届专业委员会的委员、特邀代表...     

简讯

第48届巴黎航展开幕风雨中走过百年历程2009年6月15日,第48届巴黎国际航空航天展在巴黎布尔歇国际展览中心开幕。尽管开幕当天,天公不作美,下起了大雨,但     

Solar variability and minor constituents in the lower thermosphere and in the mesosphere

Space Science Reviews - The variation in the solar irradiance related for example to the 11-year cycle leads to changes in the photodissociation and photo-ionization of the upper and middle...     

Modelling of the electromagnetic field in the interplanetary space and in the Earth's magnetosphere

A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented. In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the observational data for September 24–26, 1998 magnetic storm (Dst _min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997. This revised version was published online in August 2006 with corrections to the Cover Date.     

差值法与比值法的误差修正效果比较研究及应用

差值法与比值法对不同测量系统的误差修正效果不一样。本文将两种方法的比较用一个比值来描述,并用推得的公式进行量化表示。在进一步的应用研究中,理论分析与实验数据相互印证,同时得到许多有益的结论,有助于全面掌握测量系统的误差来源,从而灵活选择各种修正方法以获得更加准确的测量结果。     

Dust in and Around the Heliosphere and Astrospheres

Space Science Reviews - The ESA Swarm mission, launched on 22 November 2013, consists of three spacecraft each equipped with a Micro Advanced Stellar Compass ( $\mu $ ASC) from the Technical...     

Particle acceleration at the Sun and in the heliosphere

Energetic particles are accelerated in rich profusion at sites throughout the heliosphere. They come from solar flares in the low corona, from shock waves driven outward by coronal mass ejections (CMEs), from planetary magnetospheres and bow shocks. They come from corotating interaction regions (CIRs) produced by high-speed streams in the solar wind, and from the heliospheric termination shock at the outer edge of the heliospheric cavity. We sample many populations near Earth, but can distinguish them readily by their element and isotope abundances, ionization states, energy spectra, angular distributions and time behavior. Remote spacecraft have probed the spatial distributions of the particles and examined new sources in situ. Most acceleration sources can be ‘seen’ only by direct observation of the particles; few photons are produced at these sites. Wave-particle interactions are an essential feature in acceleration sources and, for shock acceleration, new evidence of energetic-proton-generated waves has come from abundance variations and from local cross-field scattering. Element abundances often tell us the physics of the source plasma itself, prior to acceleration. By comparing different populations, we learn more about the sources, and about the physics of acceleration and transport, than we can possibly learn from one source alone. This revised version was published online in August 2006 with corrections to the Cover Date.     

The Solar Wind and the Sun in the Past

Exposure to the solar wind can have significant long term consequences for planetary atmospheres, especially for planets such as Mars that are not protected by global magnetospheres. Estimating the effects of solar wind exposure requires knowledge of the history of the solar wind. Much of what we know about the Sun’s past behavior is based on inferences from observations of young solar-like stars. Stellar analogs of the weak solar wind cannot be detected directly, but the interaction regions between these winds and the interstellar medium have been detected and used to estimate wind properties. I here review these observations, with emphasis on what they suggest about the history of the solar wind.     

无损检验的现状及未来

介绍了无损检验技术的现状及对未来5～20年发展趋势的分析。无损检验技术用来对零部件进行定量测量,它包括一系列检验方法,如X射线、超声、目视、电磁、声发射、磁粉     

Discharges in the Stratosphere and Mesosphere

In the present paper salient features of discharges in the stratosphere and mesosphere (namely sprites, halos, blue starters, blue jets, gigantic jets and elves), are discussed. The electrostatic field due to charge imbalance during lightning processes may lead to stratospheric/mesospheric discharges either through the conventional breakdown based on streamers and leaders or relativistic runaway mechanism. Most (not all) of the observed features of sprites, halos and jets are explained by this processes. Development and evolution of streamers are based on the local transient electrostatic field and available ambient electron density which dictate better probability in favor of positive cloud-to-ground discharges, and thus explains the polarity asymmetry in triggering sprites and streamers. Elves are generated by electromagnetic pulse radiated by return stroke currents of cloud-to-ground/inter-cloud discharges. Generation of the both donut and pancake shape elves are explained. Electrodynamic features of thunderstorms associated with stratospheric/mesospheric discharges are summarized including current and charge moment associated with relevant cloud-to-ground discharges. The hypothesis relating tropospheric generated gravity waves and mesospheric discharges are also discussed. Finally some interesting problems are listed.     

带襟翼三维机翼上的分离流、襟翼槽与剪切口流动

本文运用嵌套网格方法严格考虑机翼切口和襟翼端面几何形状生成了合理的计算网格,并应用雷诺平均Navier-Stokes方程和Johnson-King湍流模型计算了带双襟翼三维机翼的粘性绕流,特别是大迎角下机翼襟翼上的分离流、襟翼槽与剪切口流动.计算实践表明,用该方法可以很好地预计最大升力.