引力相互作用的三个类型与总星系的泡沫结构

本研究试图表明,如将与宇宙常数有关的真空能考虑在内,就可利用牛顿力学的数学框架,将引力相互作用分为三个类型和两种表现如下:物质对物质——吸引,物质对真空——排斥,真空对真空——排斥。据此,得出了鉴别天体系统是处于膨胀状态还是处于收缩状态的一个判据。然后讨论了引力相互作用的三个类型和两种表现在总星系泡沫结构形成中的作用,认为真空能量(暗能量)扮演了起泡剂的角色。最后导出了空洞膨胀动力学方程,并对一空洞的膨胀加速度和速度进行了估计。     

《膨胀土地基上修筑机场道面对策研究》项目通过鉴定

经空后司令部批准，4月29日空后机场营房部主持召开了《膨胀土地基上修筑机场道面对策研究》项目鉴定会。该项目研究成果顺利通过技术鉴定，并得到了与会专家和领导的一致好评。《膨胀土地基上修筑机场道面对策研究》项目，系统地提出了在膨胀土上修筑机场道面的设计、试验、施工控制指标和科学的判别方法，并提供了确定经济合理的地基处理方法的有效手段，对于膨胀土地区机场工程建设顺利进行，控制投资规模，具有十分重要的意义。     

确定航空轮胎与相邻结构间隙的方法研究

本文通过对新航空轮胎的最大制造公差、使用膨胀和转动时离心力引起尺寸增长的研究，来确定航空轮胎与相邻结构的间隙，适用于军用飞机和民用飞机起落架的航空轮胎。     

大型购物中心疏散时间预测方法的对比研究

以建筑性能化防火设计为依据，以保证人员在火灾中安全疏散为目标，以环境可提供的（或者说人员可利用的）疏散时间ASET大于人员安全疏散所必需的时间RSET为原则，以某大型购物中心为例，通过日本手算法与常用的人员疏散软件SIMULEX模拟结果进行对比，分析两者在应用上的可行性。     

建筑消防安全疏散设计方法研究

建筑消防疏散至关重要，直接关系到火灾情况下人员的安全。较为系统地介绍了常用的依据规范的安全疏散设计方法和性能化安全疏散设计方法的基本思想和设计程序，比较分析了两种方法各自的优缺点，对于实际安全疏散设计中合理地选择疏散设计方法具有一定的指导意义。     

印度设想建立印度版GPS系统

印度空问研究组织(ISRO)表示，印度正在考虑研发建立印度版的GPS卫星导航系统，其基本设想是，建立由8颗卫星组成的印度区域性导航卫星系统。该项目处于计划筹备阶段，尚需政府的正式批准。     

《咬文嚼字》公布2012年十大流行语

一、正能量指的是一种健康乐观、积极向上的动力和情感。“正能量”本是物理学名词，霍金《时间简史》中就用过：“宇宙中的物质是由正能量组成的。”“正能量”的流行源于英国心理学家理查德·怀斯曼的专著《Ripitup》（中文译名《正能量》），其中将人体比作一个能量场，通过激发内在潜能，     

膨胀土地区机场场道土基施工的防治措施研究

一、前言 膨胀土在我国的分布十分广泛，在云南、广西、贵州、四川、陕西、广东、山东、河北、江苏、湖北等地均有不同程度的分布。膨胀土是指粘粒成分主要由强亲水性矿物质组成，在吸水时能表现明显的膨胀和失水时能表现明显的收缩性的高塑性粘土。在一般情况下，膨胀土的强度较高，压缩性低，多呈坚硬或硬塑状态，常被误认为是良好的地基。但由于膨胀土具有吸水膨胀、失水收缩并往复变形的性质，所以在膨胀土地区修建机场，处理不好会使土基产生溜坍、滑坡等严重事故，还会产生收缩开裂、松散、剥落等病害，从而导致道面的变形破坏。一旦出现问题，构成的破坏是不易修复的。     

“宇宙1号”6月发射升空

2005年6月21日，在巴伦支海海域，俄罗斯潜艇发射的洲际弹道导弹顶端将携带“宇宙1号”太阳帆太空飞船升空。美国行星协会同宇宙工作室联合研发的“宇宙1号”将成为第一个真正以太阳光为动力的“太空帆船”。6月15日，“宇宙1号”被安装在经改装的“波浪”洲际弹道导弹的弹头部，很快将由俄罗斯的DeltaⅢ潜艇水下发射。成功发射的“宇宙1号”经过在轨自检后，     

巴西飞机工业公司2008年飞机交付量创新高

1月16日．欧盟委员会通过了关于欧盟空中交通管制系统使用数据链接技术的新规则，以使地面空管人员和飞行器驾驶员之间更好地进行数据信息传输，实现欧盟空管系统的现代化。欧盟委员会指出，数据链接技术是地面空管人员和飞行员之间通信的一场革命，对欧洲天空中实现统一的交通管制系统现代化至关重要。数据链接技术可以允许地空之问传输书面信息，是对地空间语音通信的重要补充，     

表面介质阻挡放电等离子体体积力实验

采用粒子图像测速(PIV)技术,在2200,4800,7300,14600Pa空气压力条件下,测量了高频高压表面介质阻挡放电(surface dielectric barrier discharge,SDBD)等离子体诱导流场.根据速度场和N-S方程求解了等离子体体积力分布,分析了空气压力和激励器电压对等离子体体积力影响.实验结果表明:相同空气压力时,激励器电压越高体积力越大.相同激励器电压时,体积力随空气压力升高减小.在体积力分布区域,体积力方向一致,较大体积力区域分布于体积力方向线上游,流场高速流动区域紧挨较大体积力分布区域,位于体积力方向线下游.     

Theoretical studies of interplanetary propagation and acceleration

Studies evaluating the transport coefficients for energetic particles in interplanetary space are described in relation to particle data.In position space, the main mode of propagation is along field lines but perpendicular diffusion and drift motion is also possible. Diffusion coefficients based on interplanetary magnetic field data are either derived from quasi-linear, adiabatic theory or this theory corrected for finite scattering near 90° pitch angle or by numerical techniques. Relevant particle data includes solar proton event time profile and anisotropy measurements. In general, when Fokker-Planck transport equation solutions are fitted to particle data, the parallel diffusion coefficients obtained still appear rather larger than those given by theoretical estimates. Perpendicular diffusion is shown to be due to field line wandering and random drift motion effects. The importance of drift motion in cosmic ray modulation theory is mentioned.Although much emphasis is currently placed upon shock acceleration in CIR's, statistical acceleration in interplanetary space must be considered. Energetic particles may gain energy from longitudinal waves and cyclotron resonance interactions. Analytical and numerical estimates of the energy space diffusion coefficients are considered. Some reveal a surprising importance to this statistical acceleration and can explain a variety of data.Presented at the Fifth International Symposium on Solar-Terrestrial Physics, held at Ottawa, Canada, May 1982.     

Stochastic Acceleration of Energetic Particles in the Heliosphere

In this paper we assess possible roles of stochastic acceleration by random electric field and plasma motion in the production and transport of energetic particles in the heliosphere. Stochastic acceleration can occur in the presence of multiple small-scale magnetohydrodynamic waves propagating in different directions. Usually, this type of stochastic acceleration is closely related to particle pitch angle scattering or parallel diffusion. Given the values of the parallel diffusion coefficient inferred from the observations of cosmic ray modulation or other energetic particle phenomena in the heliosphere, stochastic acceleration by small-scale waves is much slower than acceleration by shock waves and it is also much slower than adiabatic cooling by the expansion of the solar wind; thus it is considered as inefficient for producing heliospheric energetic particles or for the modulation of cosmic rays. Another type of stochastic acceleration occurs when particles go through random compressions or expansions due to large-scale plasma motion. This acceleration mechanism could be very fast when the correlation time of the fluctuations in plasma compression is short compared to the diffusion time. Particle acceleration by an ensemble of small shock waves or intermittent long wavelength compressible turbulence belongs to this category. It tends to establish an asymptotic p ^?3 universal distribution function quickly if there is no or little large-scale adiabatic cooling. Such a particle distribution will contain an infinite amount of pressure. Back reaction from the pressure is expected to modify the amplitude of plasma waves to an equilibrium state. At that point, the pressure of accelerated particles must remain finite and the accelerated particles could approach a p ^?5 distribution function.     

Cosmic-Ray Transport and Interaction with Shocks

This paper reviews selected topics in cosmic-ray transport in the heliosphere, as well as recent insights on the interaction of cosmic rays with shocks. Topics include: (a) recent observations suggesting very long inferred scattering mean-free paths of cosmic rays, (b) recent insights into the diffusion of cosmic rays normal to a magnetic field, (c) the physics of super-diffusion and sub-diffusion, and (e) the interaction of cosmic rays with shocks moving through large-scale irregular magnetic fields.     

The Expansion of Coronal Plumes in the Fast Solar Wind

Coronal plumes are believed to be essentially magnetic features: they are rooted in magnetic flux concentrations at the photosphere and are observed to extend nearly radially above coronal holes out to at least 15 solar radii, probably tracing the open field lines. The formation of plumes itself seems to be due to the presence of reconnecting magnetic field lines and this is probably the cause of the observed extremely low values of the Ne/Mg abundance ratio. In the inner corona, where the magnetic force is dominant, steady MHD models of coronal plumes deal essentially with quasi-potential magnetic fields but further out, where the gas pressure starts to be important, total pressure balance across the boundary of these dense structures must be considered. In this paper, the expansion of plumes into the fast polar wind is studied by using a thin flux tube model with two interacting components, plume and interplume. Preliminary results are compared with both remote sensing and solar wind in situ observations and the possible connection between coronal plumes with pressure-balance structures (PBS) and microstreams is discussed. This revised version was published online in June 2006 with corrections to the Cover Date.     

Galactic effects of the cosmic-ray gas

On an astronomical scale cosmic rays must be considered a tenuous and extremely hot (relativistic) gas. The pressure of the cosmic-ray gas is comparable to the other gas and field pressures in interstellar space, so that the cosmic-ray pressure must be taken into account in treating the dynamical properties of the gaseous disk of the galaxy. This review begins with a survey of present knowledge of the cosmic-ray gas. Then the kinetic properties of the gas are developed, followed by an exposition of the dynamical effects of the cosmic-ray gas on a large-scale magnetic field embedded in a thermal gas. The propagation of low-frequency hydromagnetic waves is worked out in the fluid approximation.The dynamical properties of the gaseous disk of the galaxy are next considered. The equations for the equilibrium distribution in the direction perpendicular to the disk are worked out. It is shown that a self-consistent equilibrium can be constructed within the range of the observational estimates of the gas density, scale height, turbulent velocity, field strength, cosmic-ray pressure, and galactic gravitational acceleration. Perturbation calculations then show that the equilibrium is unstable, on scales of a few hundred pc and in times of the order 2 × 10⁷ years. The instability is driven about equally by the magnetic field and the cosmic-ray gas and dominates self-gravitation. Hence the instability dominates the dynamics of the interstellar gas and is the major effect in forming interstellar gas clouds. Star formation is the end result of condensation of the interstellar gas into clouds, indicating, then, that cosmic rays play a major role in initiating star formation in the galaxy.The cosmic rays are trapped in the unstable gaseous disk and escape from the disk only in so far as their pressure is able to inflate the magnetic field of the disk. The observed scale height of the galactic disk, the short life (10⁶ years) of cosmic-ray particles in the disk of the galaxy, and their observed quiescent state in the disk, indicate that the galactic magnetic field acts as a safety valve on the cosmic ray pressure P so that PB ²/8. We infer from the observed life and quiescence of the cosmic rays that the mean field strength in the disk of the galaxy is 3–5 × 10^–6 gauss.     

Challenges for the Advanced Composition Explorer

This report is a brief introduction to some of the vital contributions that the Advanced Composition Explorer Mission will make towards our understanding of the origins of matter and acceleration of particles on a wide range of solar and astrophysical scales. Examples of these contributions are drawn from two broad areas of the space sciences. They are: (1) Dynamical phenomena at the Sun and in the inner heliosphere; and (2) The elemental and isotopic composition of matter in the solar wind, solar accelerated ejecta, galactic cosmic radiation and the anomalous nuclear component in the heliosphere. Some current problems with theories intended to account for these phenomena are discussed, including interpretations of the stable and radioactive isotopes in the galactic cosmic rays. This revised version was published online in June 2006 with corrections to the Cover Date.     

基于体积力模型的大S弯进气道与风扇耦合计算研究

为理解超紧凑大S弯进气道与风扇的耦合效应,基于体积力模拟方法开展了一体化计算研究。研究的进气道长径比为2.5,使用Rotor 67进行耦合分析,体积力模型与冻结转子计算得到的总压比、总温比和等熵效率分别相差4.49%,0.26%和2.38%。流场分析表明,风扇对入口段流场影响较为明显,主要体现为畸变区的顺向偏转与微弱衰减;进气道出口畸变经过风扇叶片后得到改善,大低压区和反向旋流基本消失;而流体在叶片的前后缘旋流角与轴向速度的综合改变量越大,风扇对气流做功越多。总的来说,超紧凑大S弯进气道与风扇之间耦合比较明显,需要在设计时进行详细的考察。     

Cosmic Ray Isotopic Composition Studies with the Ulysses High Energy Telescope: Implications for Origin and Distribution in the Galaxy

The isotopic abundances of the Galactic cosmic radiation measured in the Heliosphere provide unique information on acceleration, propagation modes and containment times in the Galactic magnetic fields. Nuclear interactions with interstellar matter lead to observable γ-radiation production and, thus, to direct information on cosmic ray distribution throughout the Galaxy and its magnetic halo. The COSPIN High Energy Telescope (HET) has excellent isotopic resolution from hydrogen to nickel over the ten year period of Ulysses in space. Based on our recent work, we discuss the implications for modeling the acceleration and propagation of the cosmic radiation. This revised version was published online in August 2006 with corrections to the Cover Date.