光学4F系统象平面附近光强分布的研究

首先推导出光学４Ｆ系统的一般衍射变换公式，用不透明圆盘模型算出了象平面附近三维空间内的光强分布。根据计算结果，定义了象的归一化半径和象的变缘锐化率，给出了它们与粒子离物平面远场数之间的关系，从而定量地得出成象区、失真区和远场区的物理图象。最后，对粒子场测量中的粒径和空间位置测量的最小误差作了讨论。这些结果，对分析粒子的大小和分布是十分重要的，并在喷嘴雾化场测试中得到了应用。     

Interplanetary proton cumulated fluence model update

Solar particle events leading to important increase of particle fluxes at energies of order of magnitude ranging from MeV to GeV constitute an important hazard for space missions. They may lead to effects seen in microelectronics or damage to solar cells and constitute a potential hazard for manned missions. Cumulative damage is commonly expressed as a function of fluence which is defined as the integral of the flux over time. A priori deterministic estimates of the expected fluence cannot be made because over the time scale of a space mission, the fluence can be dominated by the contribution of a few rare and unpredictable high intensity events. Therefore, statistical approaches are required in order to estimate fluences likely to be encountered by a space mission in advance. This paper extends work done by Rosenqvist et al. [Rosenqvist, L., Hilgers, A., Evans, H., Daly, E., Hapgood, M., Stamper, R., Zwickl, R., Bourdarie, S., Boscher, D. Toolkit for updating interplanetary proton-cumulated fluence models. J. Spacecraft Rockets, 42(6), 1077–1090, 2005] to describe an updated predictive engineering model for the proton interplanetary fluence with energies >30 MeV. This model is derived from a complete list of solar proton fluences based on data from a number of calibrated sources covering almost three solar cycles.     

用确定性涡方法模拟二维钝体绕流

以离散涡方法为基础,采用粒子强度交换法模拟涡量扩散方程,对粒子场分布产生扭曲变形时采用粒子强度重分配,数值模拟了突然起动圆柱、风攻角为的方形截面和大海带东桥的流场,计算结果与解析解及其他数值方法计算的结果均吻合的很好,数值结果显示确定性涡方法的高精度的特性使其在模拟钝体扰流问题方面具有很大的优势.     

鸟撞飞机风挡动态响应数值模拟方法研究现状

总结了目前用于鸟撞飞机风挡动态响应的数值模拟方法,主要有解耦解法、耦合解法和光滑质点动力学法,其中耦合解法涉及接触-碰撞耦合解法和流固耦合解法。各种方法围绕鸟体（鸟撞载荷）的模拟和风挡的模拟,部分内容针对鸟撞击发动机叶片、雷达罩和垂直尾翼等,但其方法同样适用于飞机风挡,最后指出应进一步深入研究的内容。     

Study of correlations between waves and particle fluxes measured on board the DEMETER satellite

The topic of relativistic electron dynamics in the outer radiation belt has received considerable attention for many years. Nevertheless, the problem of understanding the physical phenomenon involved is far from being resolved. In this paper, we use DEMETER observations to examine the variations of the energetic electron fluxes and ELF/VLF wave intensities in the inner magnetosphere during the intense 8 November 2004 magnetic storm. Electron flux spectra and associated wave intensity spectra are analysed throughout the magnetic storm and common characteristics or differences to other storm events are retained. The overall objective of this study is to identify and derive parameters that are relevant for particle flux modelling; the time constant characterizing the persistent decay after particle enhancement was found to be one of these important model parameters.The analysis of the 8 November 2004 event reveals that for L-shell parameter higher than 4, an electron flux dropout is observed during the storm’s main phase for electrons in the energy range 0.1–1 MeV, as has been reported from other measurements. Characteristic wave spectra accompanying this phase are analysed. They show a typical enhancement in the frequency range 0.3–10 kHz at onset for all L-shell values under consideration (2 < L < 5). During the first stage of the recovery phase, the electron fluxes are increased to a level higher than the pre-storm level, whereas the level of wave intensity in the frequency range observed below 300 Hz is at its highest. In the second stage, the particle flux decrease goes hand in hand with a global wave activity decline, the relaxation time of the latter being smaller than the former’s one. In some other cases, long-lasting electron enhancement associated with constant wave activity has been observed during this latter stage. For the above mentioned storm, while at low L values the decay time constants are higher for low energy electrons than for high energy electrons, this order is reversed at high L values. At about L = 3.6 the time constant is independent of electron energy.     

海上夜间飞行的实时仿真

自然场景仿真是虚拟现实技术的重要部分,夜间海上飞行时,星空、月亮以及海面的倒影是独具特色的自然场景.为营造沉浸感强的夜海飞行虚拟现实系统,用粒子系统实现了星空的模拟,将星体动态闪烁现象演化为粒子生命的概念,并按照主导算法加扰动的思想实现星空随机性模拟;用特殊纹理融合算法模拟月亮及星月在海面的镜像,特殊纹理经过制作、着色和融合3个过程,并根据夜空景像在海面倒影的亮度衰减规律确定融合因子,将纹理和背景按照融合因子进行深度融合;最终实现了较逼真的夜海飞行虚拟现实系统.      

空间碎片超高速碰撞数值分析

采用光滑粒子流体动力学(SPH)方法对空间碎片超高速碰撞问题作了模拟分析,给出了靶孔直径和碎片云宽度随碰撞速度的变化、累积碎片分布、碎片云无量纲向前总动量随膨胀距离的变化、碎片云前端速度的变化规律以及碎片云速度矢量等。     

基于PIC方法的离子发动机光学系统粒子模拟

采用单元内粒子(PIC, Particle-In-Cell)方法对离子发动机光学系统进行了等离子体粒子模拟.PIC方法可有效地对等离子体进行粒子模拟,其中电场求解采用SOR(Successive Over Relaxation)方法,离子加速方法采用蛙跳格式.推进剂采用氙,模拟粒子为单核离子.模拟得到了栅极间电势分布、电场强度分布及栅极间氙离子数密度分布.计算结果表明,在所取的光学系统电压参数和几何参数下,粒子束能够顺利通过栅极孔,不会撞击到栅极孔壁上.粒子模拟为今后开展离子发动机光学系统腐蚀机理分析及寿命评估提供了有效的数值方法.      

平滑粒子流体动力学(SPH)方法的进展

平滑粒子流体动力学(SPH)方法是一种无网格Lagrangian计算技术,在处理一些问题时,比以Lagrangian坐标系和Eulerian坐标系为基础的常规网格有独特的优越性,特别适用于处理物质质点的流动性极大的问题,如超高速碰撞问题.文章对SPH的理论和计算方法做了简单的介绍,并对其发展过程和现状做了简单的回顾.     

FY—1C卫星空间粒子成分监测器及其探测结果

简要介绍了FY－1C星空间粒子成分监测器的任务目标、工作原理、创新特色及在轨探测结果。空间粒子成分监测器用于卫星轨道空间的带电粒子辐射监测，为卫星的在轨安全和抗辐射加固设计服务。监测器在世界上实现用1套传感器完成对高能电子、质子、α粒子至铁离子的全成分监测，使我国首次获得了870km高太阳同步轨道全空间的各种重离子分布、质子能谱分布和电子通量分布，捕捉到大量的地磁暴和太阳质子事件，获得了批重要的探测成果。