推力中止过程一维不定常气相流动数值计算

准确地预示固体火箭发动机推力中止这一瞬变过程，对飞行器飞行精度及可靠性具有重要意义。建立了一维不定常流动数值计算模型，考虑了传热、摩擦、燃面变化，燃烧室长径比、通喉比等因素，计算了推力中止过程内弹道，给出了燃气参数沿燃烧室长度的分布及随时间的变化。     

气膜冷却技术在火炮射击中的应用

炮管烧蚀一直是火炮性能提高所面临的一重大障碍，分析了火炮烧蚀的机理，提出了一种将冷却剂直接加于可燃药筒中的新型气膜冷却技术，从而在火炮内弹道性能有所提高的情况下提高了身管的使用寿命。     

超声速进气道内特性数值模拟及性能分析

采用张涵信院士提出的无波动NND格式计算了某二级斜板可调的二元混压式超声速进气道的内部湍流流场 ,较好地模拟了激波间的干扰及激波 -附面层的相互作用 ,并在解法上运用了矢通量分裂算法 ,提高计算的效率、精度和稳定性。通过数值模拟 ,预测了其内流场主要性能参数 ,并分析了飞行条件、几何尺寸调节参数等因素对其性能参数的影响     

内埋式弹舱舱门气动载荷计算分析研究

采用中心有限体积法进行空间离散和四步Runge-Kutta显式推进方法进行时间推进数值求解了非定常欧拉方程;采用Delaunay方法生成内埋式弹舱舱盖打开时的非结构网格.数值模拟了内埋式轰炸机弹舱单开舱门在分别打开8°和45°时的复杂流场.通过对上述复杂流场的分析,发现作用于舱门的气动载荷具有使其趋向于关闭的特性,且有随打开角度的增大而减小的趋势.     

Investigation on the Thermal Conductivity of 3-Dimensional and 4-Directional Braided Composites

It is vital to choose a factual and reasonable micro-structural model of braided composites for improving the calculating precision of thermal property of 3-D braided composites by finite element method (FEM). On the basis of new microstructure model of braided composites proposed recently, the model of FEM calculation for thermal conductivity of 3-dimennsional and 4-directional braided composites is set up in this paper. The curves of coefficient of effective thermal conductivity versus fiber volume ratio and interior braiding angle are obtained. Furthermore, comparing the results of FEM with the available experimental data,the reasonability and veracity of calculation are confirmed at the same time.     

90°多弯管阻力系数计算方法

为准确获得90°组合多弯管阻力系数,采用数值模拟方法对S弯管管内流动进行模拟,并通过分析归纳S弯管局部阻力的相邻影响机制及规律,提出了90°组合弯管阻力系数计算方法.研究结果表明:弯管阻力系数受2弯连接段长度影响的规律与文献试验结果一致,数值计算方法准确有效;当连接段长度大于4倍管径时,S弯管阻力系数呈线性增长;提出的90°组合弯管阻力系数计算方法考虑了多弯管间相邻影响,且采用提出的方法计算了3弯管和多弯管的阻力系数,并将结果与数值模拟结果进行了对比,二者之间的差距均在3％之内,适合工程应用.     

Probing solar and stellar interior dynamics and dynamo

Solar and stellar activity is a result of complex interaction between magnetic field, turbulent convection and differential rotation in a star’s interior. Magnetic field is believed to be generated by a dynamo process in the convection zone. It emerges on the surface forming sunspots and starspots. Localization of the magnetic spots and their evolution with the activity cycle is determined by large-scale interior flows. Thus, the internal dynamics of the Sun and other stars hold the key to understanding the dynamo mechanism and activity cycles. Recently, significant progress has been made for modeling magnetohydrodynamics of the stellar interiors and probing the internal rotation and large-scale dynamics of the Sun by helioseismology. Also, asteroseismology is beginning to probe interiors of distant stars. I review key achievements and challenges in our quest to understand the basic mechanisms of solar and stellar activity.     

QD-×××燃气轮机验证机台架试车的性能研究

QD-×××燃气轮机是由某型发动机改造成的燃气轮机,试车过程中解决了验证机起动、稳定工作并达到燃气轮机设计要求。试验数据表明:发动机改进设计后实测输出功率小于发动机设计计算功率,经过分析得出,验证机排气温度高,内涵空气流量小,是验证机输出功率小的根本原因。     

基于旋转高频信号注入法的内置式永磁同步电机低速段转子位置检测及其误差补偿

旋转高频信号注入法注入信号较为稳定,且位置估计过程不依赖电机参数,因而十分适用于内置式永磁同步电机(IPMSM)的零、低速转子位置检测。针对传统高频信号注入法无法辨别磁极的问题,用电压方波注入法检测磁极,结合有限元软件仿真,来合理选取方波电压幅值和时长,有效缩短了磁极判断耗时。分析了滤波器和信号离散化对位置估计精度的影响,提出在低速段可用线段拟合带通滤波器中心频率处的相频特性曲线,推导所需补偿角度与电机转速的关系。在理论分析的基础上,采用基于DSP28335的样机平台进行试验,结果表明磁极判断过程稳定,耗时较短,补偿后的位置估计值相比补偿前有明显改善,调速过程中系统动态性能良好。     

Fundamental (f) oscillations in a magnetically coupled solar interior-atmosphere system – An analytical approach

Solar fundamental (f) acoustic mode oscillations are investigated analytically in a magnetohydrodynamic (MHD) model. The model consists of three layers in planar geometry, representing the solar interior, the magnetic atmosphere, and a transitional layer sandwiched between them. Since we focus on the fundamental mode here, we assume the plasma is incompressible. A horizontal, canopy-like, magnetic field is introduced to the atmosphere, in which degenerated slow MHD waves can exist. The global (f-mode) oscillations can couple to local atmospheric Alfvén waves, resulting, e.g., in a frequency shift of the oscillations. The dispersion relation of the global oscillation mode is derived, and is solved analytically for the thin-transitional layer approximation and for the weak-field approximation. Analytical formulae are also provided for the frequency shifts due to the presence of a thin transitional layer and a weak atmospheric magnetic field. The analytical results generally indicate that, compared to the fundamental value ($\omega =\sqrt{\mathit{gk}}$), the mode frequency is reduced by the presence of an atmosphere by a few per cent. A thin transitional layer reduces the eigen-frequencies further by about an additional hundred microhertz. Finally, a weak atmospheric magnetic field can slightly, by a few percent, increase the frequency of the eigen-mode. Stronger magnetic fields, however, can increase the f-mode frequency by even up to ten per cent, which cannot be seen in observed data. The presence of a magnetic atmosphere in the three-layer model also introduces non-permitted propagation windows in the frequency spectrum; here, f-mode oscillations cannot exist with certain values of the harmonic degree. The eigen-frequencies can be sensitive to the background physical parameters, such as an atmospheric density scale-height or the rate of the plasma density drop at the photosphere. Such information, if ever observed with high-resolution instrumentation and inverted, could help to gain further insight into solar magnetic structures by means of solar magneto-seismology, and could provide further insight into the role of magnetism in solar oscillations.