梁/液体耦合振动的边界积分对称列式法

 利用格林积分导出的液体内部扰动压力函数作为测试函数,通过变分得到一组具有对称系数的代数方程,将该方程同梁的有限元振动方程联立后,即可求解梁在液体中的耦合振动问题。本方法具有未知数目少,数据存储和计算效率高的特点。     

相关技术微分动力模型及定性分析

 本文建立了由两个相关技术组成的技术系统的微分动力模型。用微分方程定性理论讨论了系统的平衡点及系统在平衡点处的稳定性。在相平面和时间图上给出了几种典型的技术发展模式。     

压缩拐角区的压力,热流工程计算方法

 <正> 引言 从压缩拐角分离流动的试验及数值计算出发,建立起一个实用范围较广精度较高的工程估算程序,方便快速地估算出压缩拐角分离区和再附区的峰值压力、峰值热流;分离区和再附点位置;分离区长度等。这是气动设计部门关注的课题。这些工作是在文献(3,4)中的经验公式的基础上,按照分离流动流谱,分区进行迭代修正计算,对二维情况给出了完整     

马赫数对后掠激波和湍流边界层干扰特性的影响

本文介绍了尖前缘翼诱导激波和湍流边界层干扰流场壁面特性，着重强调马赫数影响。给出２．０≤Ｍ≤８．２、ａ≤３５°分离流场中，锥型干扰区内主分离线和再附线位置与无粘激波角β０和迎角ａ的相关式，证实无粘条件是控制锥型区尺度的主要因素，面高超声速与超声速干扰流中二次分离随激波强度的不同发展，表明干扰流场的细致结构与可压缩性有关。     

绕凸台的高超声速分离流动研究

本文研究高超声速流动绕三维低凸台的流动特性。凸台高度与边界层厚度之比介于0.5～0.8,凸台周边倾角介于14°～45°。在高超声速风洞中,来流马赫数为5,单位雷诺数为2.6～6.0×10~7/米。实验过程中测量了模型中心线及特殊部位之表面压强分布,根据纹影记录及表面流动显示确定激波与边界层干扰流场特性及分离区的变化。发现分离区在中心线上距凸台最远,而在凸台肩部距周边沿法线方向最近,确定了中心线上最大压强比的位置。     

后掠压缩角激波边界层柱形干扰研究

本文给出了由后掠压缩角模型引起的激波和湍流边界层干扰的实验研究结果,着重提出了柱形干扰中的尺度特性。本实验中的马赫数为1.79,2.04和2.50,相应的雷诺数为2.42～2.47×10~7/米。模型后掠角的变化范围是0°到60°,流向压缩角的变化范围为0°到30°。实验结果表明,在本实验的马赫数范围内,干扰流动的上游影响区呈现柱形或锥形,如果考虑横流效应,柱形干扰区的上游影响尺度能和二维压缩角的上游影响尺度相关联。其相关关系仅受后掠角和来流马赫数的影响,而与压缩角大小无关。     

平板上直立圆柱引起的三维湍流分离流的传热特性

 1.实验目的与方法 航天飞行器再入大气层时,其表面突出物引起的三维湍流分离,使局部热流急剧增加。突出物激波与湍流边界层的干扰流场很复杂,需要较多的测量数据揭示其流动规律。为此,在激波风洞中Ma_1=5.2,Re/L=2.3×10~7m~(-1)的气流条件下,测量了平板上直立圆柱干扰区中柱前缘及其邻近平板上的热流分布,并拍摄了激光纹影     

贮箱液固耦合振动分析的数值研究

 <正> 线性液固耦合系统有限元分析的理论研究比较充分。但有关理论结果的数值研究仍需深入,以便能生成工程中实用的有限元液固耦合分析系统。位移法(或拟弹性法)因其零能模式的分离问题,带来了实用上的困难。压力-位移模式需要对有限元矩阵对称化。lrons曾提出一种对称化方法,但在数值实施中往往无法应用。文献[2]、文献[6]曾给出了另外三种对称化途径,但还没有进行数值上的探讨。本文目的在于探讨数值上可行的对称化方法,生成有关程序块.以便发展成为压力-位移模式的工程应用软件。作为算例,研究了贮箱的耦合振动问题,重点考虑了自由面波的影响。     

One-up on L1: Can X-rays provide longer advanced warning of solar wind flux enhancements than upstream monitors?

Observations of strong solar wind proton flux correlations with ROSAT X-ray rates along with high spectral resolution Chandra observations of X-rays from the dark Moon show that soft X-ray emission mirrors the behavior of the solar wind. In this paper, based on an analysis of an X-ray event observed by XMM-Newton resulting from charge exchange of high charge state solar wind ions and contemporaneous neutral solar wind data, we argue that X-ray observations may be able to provide reliable advance warning, perhaps by as much as half a day, of dramatic increases in solar wind flux at Earth. Like neutral atom imaging, this provides the capability to monitor the solar wind remotely rather than in situ.     

Propagation of interplanetary shocks into the Earth’s magnetosphere

This paper is devoted to the study of propagation of disturbances caused by interplanetary shocks (IPS) through the Earth’s magnetosphere. Using simultaneous observations of various fast forward shocks by different satellites in the solar wind, magnetosheath and magnetosphere from 1995 till 2002, we traced the interplanetary shocks into the Earth’s magnetosphere, we calculated the velocity of their propagation into the Earth’s magnetosphere and analyzed fronts of the disturbances. From the onset of disturbances at different satellites in the magnetosphere we obtained speed values ranging from 500 to 1300 km/s in the direction along the IP shock normal, that is in a general agreement with results of previous numerical MHD simulations. The paper discusses in detail a sequence of two events on November 9th, 2002. For the two cases we estimated the propagation speed of the IP shock caused disturbance between the dayside and nightside magnetosphere to be 590 km/s and 714–741 km/s, respectively. We partially attributed this increase to higher Alfven speed in the outer magnetosphere due to the compression of the magnetosphere as a consequence of the first event, and partially to the faster and stronger driving interplanetary shock. High-time resolution GOES magnetic field data revealed a complex structure of the compressional wave fronts at the dayside geosynchronous orbit during these events, with initial very steep parts (10 s). We discuss a few possible mechanisms of such steep front formation in the paper.