动目标双站RCS预估的图形电磁计算（GRECO）方法

图形电磁计算 (GRECO)技术是目前分析高频区复杂目标雷达散射截面 (RCS)最有效方法之一。通过应用 GRECO方法和单 -双站等效原理 ,计算动目标高频区的双站 RCS,给出了与实验结果符合良好的计算实例 ,具有很好的工程应用价值     

抽吸孔板的气动实验及附面层抽吸数值模拟

 为了给附面层抽吸提供可靠的抽吸边界条件 ,通过对孔板厚径比t/d =0.1～ 2.67,开孔率ε =6.3%～ 23%的多孔板进行实验 ,建立了附面层抽吸孔板小孔马赫数与孔板前后压差、孔板厚径比、孔板开孔率间的关系。发现随着孔板前后压差的加大 ,小孔马赫数增加 ,当孔板前后压差达到一定值时 ,小孔发生壅塞 ,小孔马赫数不再变化 ,孔内流动达到壅塞状态。与此同时 ,总结出了附面层抽吸孔板小孔马赫数的经验公式。为了进一步检验所得经验式的准确性 ,还用实验所得经验式作为附面层抽吸边界条件 ,对来流马赫数分别为1.98,1.58和 0.8三种情况下的附面层抽吸流场进行了数值模拟。计算结果准确反映了超声来流和亚声来流条件下的附面层抽吸的流动特征 ,抽吸流量与Willis和Syberg的实验结果吻合较好 ,表明给定的附面层抽吸边界条件是正确、可行的。     

硅氧氮陶瓷的先驱体法合成及性能的研究

用 Si Cl4为原料 ,通过水解和氨解的方法 ,制备了不同含氮量的硅氧氮先驱体。先驱体通过脱氨基原位聚合 ,再经过无机化转变成为成分均匀的硅氧氮粉体 ,用所得粉体热压烧结制备了硅氧氮材料。测试分析结果表明 ,氮的引入使氧化硅的析晶温度提高了 1 5 0℃ ;适量析晶显著提高材料的力学性能 ;烧结温度为 1 4 0 0℃时 ,氮的质量分数为 2 4 .3%材料的强度和韧性最大 ,分别达到 1 5 6 MPa和 1 .8MPa· m1 / 2 ,比 Si O2 基体的强度和韧性提高了 4 .5 8倍和 2 .2 5倍。     

Three-dimensional plasma measurements within the earth's magnetosphere

First magnetospheric measurements of the three-dimensional velocity distributions for positive ions and electrons within the energy range 1 eV E/Q 45keV are reported. These velocity distributions are gained with quadrispherical Lepedeas on board the spacecraft ISEE-1 and -2. Three-dimensional bulk flows of protons in the vicinity of the magnetopause and within the dayside magnetosphere and dawn sector of the magnetotail are presented. Proton drift velocities within the magnetosphere and magnetotail can be directly determined and employed to calculate the corresponding quasi-static perpendicular electric fields and to provide quantitative analyses of kinematical models for plasma motions. Nonmonotonic features in the electron velocity distributions are found simultaneously with the presence of electron cyclotron harmonic electrostatic waves in the dayside magnetosphere. The relationship of the observed electron velocity distributions to expectations for resonant pitch-angle and energy diffusion is discussed, as well as the possibility of the existence of proton cyclotron harmonic instabilities. Examples of the signature of field-aligned acceleration of protons into the magnetosphere and the presence of low-energy ionospheric ions in the near-earth magnetotail are also presented. Perpendicular electrostatic fields can be calculated from the observed three-dimensional velocity distributions and are found to have typical magnitudes of 1 mV m^-1.     

航空结构件铣削残余应力分布规律的研究

 采用三维有限元方法,模拟计算航空铝合金7050-T7451 材料在无内应力前提下数控铣削时产生的表层残余应力场。在综合考虑了现行的常规工艺方案基础上,从中选定4 种具有代表性的走刀路径分别进行分析计算,进而优选出最为合适的走刀工艺规则。走刀过程采用动态载荷步模拟,材料去除采用生死单元模拟,从而使计算结果更加精确、可信。通过本文的研究工作,可为提高该类材料数控铣削加工的尺寸稳定性确定合理的工艺策略。     

混压式进气道与弹体一体化流场数值模拟

基于Favre平均的N－S方程和B／L代数湍流模型,采用Jameson格式和矩阵人工粘性,对X布局的混压式超声速进气道与弹体的一体化流场进行了数值模拟,研究了解决了数值计算中的附面层抽吸及混压式进气 启动问题,得出了进气道内外流场的马赫数分布和速度分布,讨论了绕弹体非均匀来流条件下,进气道的位置,附面层抽吸及攻角对进气道性能的影响和进气道外型形状对弹性气动力的影响,结果表明,对混压式进气道必须进行附面层抽吸,进气道的位置对进气道的性能有很大的影响,进气道的外型型面对弹体的气动性能有一定的影响。     

歼击机高度分层试飞验证

针对采用气动补偿空速系统以改善测高系统精度的现代飞机 ,简要介绍了高度分层的要求 ;阐述了引起飞机空速系统位置误差的主要误差源并进行了分析 ;给出了通过 GPS速度法对歼击机高度分层试飞验证结果 ,并对试飞结果进行了分析和讨论 ;结果表明 ,所得到的试飞数据可为飞机气动补偿空速系统设计和高度分层试飞方法研究提供重要依据。     

The evolution of massive stars

The evolution of stars with masses between 15 M ₀ and 100M ₀ is considered. Stars in this mass range lose a considerable fraction of their matter during their evolution.The treatment of convection, semi-convection and the influence of mass loss by stellar winds at different evolutionary phases are analysed as well as the adopted opacities.Evolutionary sequences computed by various groups are examined and compared with observations, and the advanced evolution of a 15M ₀ and a 25M ₀ star from zero-age main sequence (ZAMS) through iron collapse is discussed.The effect of centrifugal forces on stellar wind mass loss and the influence of rotation on evolutionary models is examined. As a consequence of the outflow of matter deeper layers show up and when the mass loss rates are large enough layers with changed composition, due to interior nuclear reactions, appear on the surface.The evolution of massive close binaries as well during the phase of mass loss by stellar wind as during the mass exchange and mass loss phase due to Roche lobe overflow is treated in detail, and the value of the parameters governing mass and angular momentum losses are discussed.The problem of the Wolf-Rayet stars, their origin and the possibilities of their production either as single stars or as massive binaries is examined.Finally, the origin of X-ray binaries is discussed and the scenario for the formation of these objects (starting from massive ZAMS close binaries, through Wolf-Rayet binaries leading to OB-stars with a compact companion after a supernova explosion) is reviewed and completed, including stellar wind mass loss.     

Solar flares as sources of energetic particles

In this paper a review is presented of the present status of our knowledge of solar flare phenomena with special emphasis on the production of suprathermal particles and their solar effects. Of these energetic particles electrons play an important role since they produce the X-ray and radiobursts observed during many flares. Also, during their slowing down to thermal energies they contribute to the heating of localized regions in the solar atmosphere, through energy exchange with the ambient electrons. Observable radiations of energetic protons, and other nuclei, are produced through nuclear interactions leading to the emissions of gamma-ray lines. Detectable fluxes of these gamma-ray lines are produced only in the most powerful flares. Also the nuclei that enter into deeper layers of the solar atmosphere transfer most of their kinetic energy to the ambient plasma.