等厚度楔形杆的应力分析

本文将应力场分为基本应力场和修正应力场两个部分。基本应力场的应力σ_x用勒让德级数展开,级数的前两项系数用截面法确定;其他应力τ_(xy),σ_y由平衡方程和侧表面边界条件确定;再用余能原理确定其余各项系数。由于该级数收敛很快,故可得到封闭解并能给出该解的应用范围,为精确满足自由端的静力边界条件,又引入一个从自由端到固定端迅速衰减的修正应力场,该应力场的应力在自由端等于已知外力与基本应力解之差。其确定方法与基本应力场相同,它也有一个封闭解。将以上两应力场相加卽可得到满足全部边界条件的解。     

无界域上不定二次规划的一个算法

本文给出了无界域上不定二次规划一个算法。该算法将不定规划转化为一系列凸二次规划，并证明了算法的收敛性。     

二维粘性不可压缩流场的分块耦合求解方法

本文用分块耦合的方法，并采用S.Abdallah^[1,2]和M.L.Mansour^[3]的在非交错网络上隐式求解原始变量的Navier-Stokes方程的提法和离散格式，成功地解决了二维复杂流场的数值求解问题，获得了空腔流、T型叉管流、NACA0020翼型绕流和方块钝体绕流的稳态解，并进行了讨论。此方法还可推广到三维复杂流场的计算问题。     

Phase Space Density Analysis of Energy Transport in the Earth’s Magnetotail

Two energetic events in the Earth’s magnetotail detected by Geotail are examined with detailed analysis of three-dimensional velocity phase space density. It is found that the occurrence of multiple ion components is high during these dynamic episodes. Different populations evolve independently of each other, suggesting particles from multiple activity sites contributing to the observed phase space density. The transport properties with consideration of multiple components are evaluated, with the result showing significant differences from those based on a single fluid approach. This comparison indicates that precise evaluation of the energy and magnetic flux transport of energetic events in the magnetotail requires resolving individual populations in the phase space density.     

跨音速小扰动方程的多重解

本文利用Engquist-Osher格式,离散跨音速小扰动方程(TSD)和边界条件,选择不同初场计算NACA0012翼型二维定常位势流场,得到了与试验值较符合的结果,同时用Murman-Cole非守恒和守恒两格式计算并进行了比较。着重用数值实验进一步探讨多重解问题,发现并总结出了几点很有参考价值的规律和现象。     

在火箭发动机燃烧室中气相湍流流动的理论计算

本文用单流体湍流模型对液体火箭发动机突扩燃烧室中冷态气相流动的速度场和湍流强度分布进行了数值计算并与实验数据进行了对比和分析.     

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。     

一种多目标随机决策方法及其应用

本文通过引进决策方案的可行度和决策者参考目标水平的满足度等概念,提出了一种不确定条件下的多目标随机决策方法——交互式参考目标满足度与可行度决策分析中,取得了较好的效果。     

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。