Instability and unsteadiness of aircraft wake vortices

This paper presents a review of theoretical and experimental results on stability and other unsteady properties of aircraft wakes. The basic mechanisms responsible for the propagation and the amplification of perturbation along vortices, namely the Kelvin waves and the cooperative instabilities, are first detailed. These two generic unsteady mechanisms are described by considering asymptotic linear stability analysis of model flows such as vortex filaments or Lamb–Oseen vortices. Extension of the linear analysis to more representative flows, using a biglobal stability approach, is also described. Experimental results obtained using LDV, hot wire and PIV in wind tunnels are presented and they are commented upon the light of theory.     

高超声速无粘流场的推进计算

本文将文[1]中用于时间相关法计算的NND格式推广到定常超声速流动的空间推进计算,采用二步的预测、校正方法保证了推进方向的二阶精度,可以证明,这种二阶精度的NND格式具有TVD性质,是MacCormack二步显式格式的推广。本文首先将格式应用于二维平板上斜激波反射流场的推进计算,以检验格式捕捉激波的能力,同时研究了不同的通量分裂方法对格式捕捉激波能力的影响,得到了相当满意的结果。在此基础上,计算了航天飞机简化外形的身部超声速流场,给出了M_∞=10,α=0°,和M_∞=5,α=5°两种状态的部分结果,计算结果清楚地描绘了由于气流在机翼附近受到强烈压缩而产生的内嵌激波与外激波相交的复杂流场结构,与文[7]相比,流场结构更为清晰。     

作为企业组织形式的信托

在信托作为企业组织形式的发展过程中,有两个问题值得关注：一是为什么信托能够作为企业的组织形式;二是信托作为企业组织形式经历了由盛而衰,然后再度崛起的过程,其背后的原因是什么？以法经济学的视角观察会发现,信托与公司在资产分割及其所导致的债权人模式上是没有区别的,这奠定了信托作为企业形式的基础;而以企业理论观察,就会发现信托与公司在企业所有权安排上的不同,即信托将控制权安排给了人力资本所有者,而公司则是将控制权安排给了非人力资本,这一不同导致了两者在治理结构与应用范围上的差别。     

2007年我国经济社会又好又快发展的市场机制和制度保证

2007年是我国发展和改革的关键之年，中央经济工作会议提出的从“又快又好”发展到“又好又快”发展的政策转变，意味着我国经济社会发展进入了新时期。为此，我们必须坚持以科学发展观统领经济社会发展全局，并切实将其落实；在宏观调控中完善市场机制，加快经济增长方式的转变；加快领导制度、组织制度、考核制度建设，发挥制度的综合效应，同时考虑制度实施的成本和环境。努力实现速度、质量、效益相协调，消费、投资、出口相协调，人口、资源、环境相协调，真正从经济发展的“又快又好”迈向“又好又快”。     

关联性与文化的解读和建构

根据Sperber和Wilson的关联理论及其认知语境观,说明外语读者如何在认知语境中寻找最佳关联,可以对作者所设置的文化缺省进行连贯解读,从而实现跨文化图式的建构。     

对邓小平民主理论的几点阐析

邓小平的民主理论是马克思主义同中国实际相结合的产物。它在坚持马克思主义民主理论基本原理的基础上 ,作了进一步的丰富和发展。作者对其有关民主理论的新理论加以阐析。     

企业自我评价方法的层次模型

通过分析比较ISO9000:2000标准和质量奖模型,对应马斯洛的需求层次提出了企业自我评价方法的层次模型,揭示了ISO9000标准和质量奖模型作为企业自我评价方法的层次逻辑关系,即两者互相补充,一方面以ISO9000标准为基础,通过PDCA循环反映企业运作的变化和改进;另一方面,在ISO9000标准的基础上通过质量奖准则,找出企业优势,在此基础上,继续改进.     

攻击活动目标的一种最优弹道估计

 为分析活动目标的随机飞行状态和减小导弹的脱靶量,提出了数学模拟打靶的一种新方法。其中包括卡尔曼滤波理论结合最大似然法的应用,以及建立相对运动的离散化模型和灵敏度矩阵。为改善飞行状态的估计精度,论述了确立飞行弹道修正协方差矩阵的概念。除此之外,还讨论了导引敏感器静态误差影响脱靶量的估计问题。     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

可重复使用运载器磁悬浮助推发射参数研究

针对磁悬浮助推水平起飞运载器这种新型发射概念,采用概念性分析方法,研究地面发射参数对可重复使用运载器性能的影响规律。结果表明,助推发射水平起飞运载器在降低初始推重比、推进剂和结构质量等方面具有优势,最后得出地面发射参数的一组优化值。