室火轰燃的大涡模拟

采用一套修正的适用于低马赫数浮力流的N-S方程组来描述火灾场,运用Smagorinsky亚格子模型的大涡模拟方法对室内池火的轰燃发展过程进行了数值模拟,把模拟与实验结果进行了对比和分析。结果表明,该方法能较好地预测轰燃。同时模拟结果显示火焰区向房间后部偏转稍大,近壁处温度预测的误差大一些,随着亚格子模型的不断完善和计算能力的提高,用该技术来预测轰燃现象会更加准确。     

微型凸起物高超声速气动热特性研究

利用N-S数值解方法对高超声速气流中微型凸起物的气动热环境进行了计算研究,并对前斜坡峰值压力和热流跃升进行了分析,结果表明对于高雷诺数流动,由于其边界层很薄,气流对凸起物的冲击作用比低雷诺数流动大很多,给凸起物前缘和上表面带来较严重的气动热问题。研究还表明利用斜面侧扩张角可以降低凸起物后斜坡的气动热环境。最后对球锥与平板物型的差异给微型凸起物热环境特性带来的影响进行了研究,结果表明在本文计算状态下,风洞平板实验模型得到的凸起物前缘峰值压力和热流跃升比实际球锥外形要高,因此地面实验结果外推到天上实际情况还是比较保守的。     

论社会主义市场经济条件下的按劳分配

我国现阶段实行的按唠分配不是马克思原意的按劳分配，而是按社会必要劳动时间分配，是按劳分配原则在社会主义市场经济条件下的转化形式。按社会必要劳动时间分配的实质是按生产要素分配。     

高深径比TC4钛合金筒形件普旋成型有限元数值模拟

采用有限元法对特定高深径比TC4钛合金筒形件普旋成型进行了数值模拟,分析了运动轨迹、旋压道次间距和间隙对成型的影响.结果表明普旋时坯料不同部位的应力应变状态不同,采用凹曲线轨迹,间隙为3.5 mm,首道次间距为9 mm,分6道次旋压成型效果好.同时在有限元数值模拟基础上,成功旋制了高精度试验件,说明有限元模拟对旋压具有很好指导意义.     

基于HLA的空地作战分布交互式仿真系统研究

文中在对HLA和RTI进行简介的基础上,以建立空地作战仿真系统为背景,论述了基于HLA的空地作战仿真系统的设计思想及开发过程。     

分布式航空兵突击作战仿真系统开发

现代战争已发展到海、陆、空、天、电磁多维空间作战,仿真技术在军事上的应用对作战行动起着重要的指导作用。文中运用目前流行的分布式交互仿真思想,设计了分布式海军航空兵突击作战仿真系统,并对相关联邦成员以及预警机CGF进行了开发,对分布式作战系统的开发具有参考价值。     

液体火箭发动机试验台贮箱增压系统模块化仿真

采用一维理想气体流动的有限元状态变量模型,运用模块化建模与仿真方法和Fortran90语言进行了某液体火箭发动机试验台贮箱增压系统工作过程的仿真,获得了细致的管网状态参数分布曲线,为分析贮箱增压系统的工作过程及各组件的作用提供了数值依据。数学模型和模块化建模与仿真方法显示出较好的有效性和通用性。      

二维涡轮叶栅流场的直接数值模拟

采用高精度有限差分格式求解非定常N-S方程组,对低雷诺数下二维涡轮叶栅流动进行了直接数值模拟,计算了雷诺数为10000,VKI涡轮叶栅在0°,8°以及-8°攻角下的流场,对涡轮叶栅非定常流动机理做了初步的探讨。计算结果表明:在叶栅尾缘处,逆时针方向和顺时针方向的主涡交替在壁面产生,并和主流相互作用产生二次涡,而当二次涡与主流连通发生掺混时,将引起主涡被分割并从叶片表面脱落;攻角在一定范围内的变化对VKI涡轮叶片表面边界层发展影响不明显。文中还对尾迹区的统计量特性和速度亏损特性等进行了研究。      

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.