固冲发动机补燃室内强迫对流条件下硼颗粒燃烧速率研究

硼颗粒在通过固体火箭冲压发动机的燃气发生器喷管进入补燃室的过程中,颗粒通常都会受到高速气流的作用。此时,静止条件下硼颗粒的燃烧模型不再适应。对强迫对流条件下的硼颗粒燃烧的二维问题建立了数学模型,通过物理、数学简化,将偏微分方程组化为易于求解的常微分方程组,最后得到燃烧速率的显示表达式,并进行了求解,给出了硼颗粒周围边界层内温度场、浓度场及颗粒燃烧速率随雷诺数Re的变化规律。     

基于改进粒子群算法的高超声速飞机爬升轨迹优化

装备涡轮基组合动力发动机的高超声速飞机,其推力特性不同于传统的涡扇发动机,因此传统飞机的爬升策略不再适合这类高超声速飞行器。在分析了飞机爬升段数学模型的基础上,基于改进粒子群优化算法针对某高超声速飞机模型飞行剖面爬升段,以最小燃油消耗为目标进行轨迹优化设计。通过仿真计算,优化后的爬升段飞行轨迹能有效减少燃油消耗,证明了优化方法的可行性。     

基于粒子群寻优的高精度星敏感器在轨标定方法

星敏感器结构设计与安装过程会产生多种误差,主要误差源有星敏感器像平面主点误差、主距误差、倾斜误差与旋转误差,这些误差影响了星敏感器在轨标定的精度。本文根据星敏感器的误差模型,提出了一种高精度的星敏感器在轨标定方法。在已知含有误差的像平面的基础上,构造一个虚拟的像平面。当粒子群优化算法使含有误差的像点投影到虚拟像平面上的坐标与无误差时像点的坐标一致时,再利用Quest解算出三轴姿态角求得两个像平面之间的姿态矩阵,得出两像平面之间的关系。结果表明：星敏感器姿态确定精度较高且比较稳定。这种方法与传统标定方法的优势在于不依靠陀螺信息,原理简单,提高了数据的准确性。     

充液挠性航天器姿态机动控制的多目标优化

针对充液挠性航天器姿态快速机动、快速稳定的控制要求,为减小姿态机动对挠性附件振动和液体晃动的激发,设计了一种基于正弦型加加速度的姿态机动路径规划方法。为进一步提高姿态控制性能,提出了一种基于云多目标粒子群算法的姿态控制器参数和机动路径参数联合优化方法。以最小化充液挠性航天器三轴姿态达到指定指向精度的时间以及三轴姿态稳定度,构建多目标优化模型,并应用云多目标粒子群算法求取姿态控制器参数和机动路径参数的Pareto最优解。仿真结果表明:采用多目标联合优化算法得到的控制器与路径参数,能够有效减小液体晃动和挠性附件振动,显著提高充液挠性航天器大角度姿态机动的快速性和稳定性。     

SiC颗粒强韧化MoSi2复合材料研究

本文通过对热压合成制备的SiC MoSi2 复合材料显微组织及其断口形貌分析 ,结合硬度、抗弯强度、断裂韧度等力学性能和孔隙率、晶粒度的测试 ,初步探讨了SiC颗粒强韧化MoSi2 复合材料的效果和机制。     

粒度和形貌及粒度分布对RDX安全和热分解性能的影响

采用溶剂/非溶剂法和筛分法,通过控制搅拌速度及溶剂与非溶剂温度差,制备了不同粒度、形貌和粒度分布的RDX粉末。利用激光粒度仪、扫描电子显微镜(SEM)和X射线衍射(XRD)对其进行了相应表征;利用撞击和摩擦感度试验、慢烤试验及DSC测试分别研究了不同粒度、形貌及粒度分布的RDX样品的安全性能和热分解特性。研究结果表明,粒度、形貌及粒度分布是影响RDX安全和热分解性能的重要因素。随着粒度的减小,RDX的机械和热感度显著降低。另外,窄粒度分布的RDX样品普遍具有更低的机械感度,而宽粒度分布的RDX样品通常具有更好的热稳定性。     

Magnetic energy release near accreting black holes

The observed non-thermal emission from accreting compact objects is often understood in terms of the expected magnetic activity of accretion disks. This review discusses the constraints on this view point that can be obtained from, principally, the X-ray spectra and the X-ray variability of black hole candidates.Furthermore, the traditional view of an accretion disk corona, put forward as the source of the non-thermal emission, analogous to the solar corona is shown to be wrong on a few important points. Firstly, the density in the equilibrium accretion disk corona is extremely low. A reasonable plasma density is retained by pair production processes similar to those existing in the pulsar magnetosphere. Secondly, the dominant resistivity in the accretion the disk on the current carrying electrons.     

Particle acceleration and kinematics in solar flares – A Synthesis of Recent Observations and Theoretical Concepts (Invited Review)

We review the physical processes of particle acceleration, injection, propagation, trapping, and energy loss in solar flare conditions. An understanding of these basic physical processes is inexorable to interpret the detailed timing and spectral evolution of the radiative signatures caused by nonthermal particles in hard X-rays, gamma-rays, and radio wavelengths. In contrast to other more theoretically oriented reviews on particle acceleration processes, we aim here to capitalize on the numerous observations from recent spacecraft missions, such as from the Compton Gamma Ray Observatory (CGRO), the Yohkoh Hard X-Ray Telescope (HXT) and Soft X-Ray Telescope (SXT), and the Transition Region and Coronal Explorer (TRACE). High-precision energy-dependent time delay measurements from CGRO and spatial imaging with Yohkoh and TRACE provide invaluable observational constraints on the topology of the acceleration region, the reconstruction of magnetic reconnection processes, the resulting electromagnetic fields, and the kinematics of energized (nonthermal) particles. This revised version was published online in June 2006 with corrections to the Cover Date.     

Gamma-rays from Active Galactic Nuclei: Emission processes and particle acceleration

It is argued that the high-energy X-ray and -ray emission from flaring blazars is beamed radiation from the relativistic jet supporting the relativistic beaming hypothesis and the unified scenario for AGNs. Most probably the high-energy emission results from inverse Compton scattering by relativistic electrons and positrons in the jet of radiation originating external to the jet plus pair annihilation radiation from the jet. Future positive TeV detections of EGRET AGN sources will be decisive to identify the prominent target photon radiation field. Direct -ray production by energetic hadrons is not important for the flaring phase in -ray blazars, but the acceleration of energetic hadrons during the quiescent phase of AGNs is decisive as the source of secondary electrons and positrons through photo-pair and photo-pion production. Injection of ultrahigh energy secondary electrons and positrons into a stochastic quasilinear acceleration scheme during the quiescent AGN phase leads to cooling electron-positron distribution functions with a strong cut-off at low but relativistic energy that under certain local conditions may trigger a plasma instability that gives rise to an explosive event and the flaring -ray phase.     

应用混合网格分析复杂积冰翼型气动性能

通过发展一种点-点对接的结构/非结构混合网格生成方法,避免了复杂积冰外形难以划分结构化网格的问题,并对复杂积冰翼型的气动性能进行了分析计算.在靠近积冰边界的内层采用了非结构网格以拟合复杂的边界,在非结构网格外采用结构化网格以节省存储空间和计算时间.为了检验网格对选用湍流模型的影响,整个流动区域分别采用SST和SA湍流模型,求解了雷诺平均N-S方程.数值计算结果表明SST模型更适于模拟复杂分离流动,积冰对翼型的气动性能造成了严重的影响.