水下超声速射流对上浮水雷受力特性影响研究

固体火箭发动机具有功率密度大、推力大等优势,常被用于上浮水雷的推进器。然而发动机在水下工作时燃气射流使流场压力发生剧烈脉动,进而影响发动机的推力性能及上浮水雷的受力特性。基于VOF多相流模型和理想气体模型,建立了上浮水雷在不同工作状态(欠膨胀、完全膨胀、过膨胀)下的数值模型,研究了水下燃气喷射流对上浮水雷的受力特性影响。结果显示,欠膨胀工况时,发动机推力平缓,大小为12.2KN,上浮水雷受力未出现负值;完全膨胀时,射流发生颈缩、胀鼓现象位置距离雷体较远,导致发动机推力及水雷壳体受力振荡不剧烈;过膨胀工况时,射流发生颈缩、胀鼓现象距离喷管较近,发动机推力发生剧烈脉动,产生21.37%的振荡幅度,胀鼓现象发生时,流场压力显著降低使得上浮水雷后体受力减小,壳体阻力增大,上浮水雷最大产生27KN的负推力。     

展向振荡对激波/湍流边界层干扰的影响

周期振荡作为一种有效的壁面流动控制手段受到广泛关注,而其对激波/湍流边界层干扰的影响目前鲜有研究。本文采用高精度直接数值模拟（DNS）方法对马赫数2.9、12°激波入射角、强振荡下的激波/湍流边界层干扰进行了系统研究。通过与无振荡工况的定量比较,揭示了展向强振荡对干扰区内复杂流动结构的影响规律及作用机制,如分离泡尺度、物面压力脉动非定常特性、物面剪切的非定常特性及统计特征等。研究发现：在展向强振荡作用下,分离点位置提前,间歇区长度增大;同时由于分离泡内强黏性耗散的影响,展向振荡的穿透高度约为分离泡高度的4%,因而对流动结构不会产生实质影响。但展向强振荡会对壁面附近流动造成显著影响,如强振荡诱导的壁面展向速度远大于流向速度,造成流向剪切与展向剪切之间夹角的概率密度函数峰值从0°偏移到80°~90°之间。物面压力及剪切本征正交分解分析表明,展向振荡会导致模态能量从低阶模态向高阶模态转移,降低低频运动的能量占比,增强再附后Görtler涡等壁面附近旋涡结构的强度。     

推力室状态对其声学振型及其阻尼特性的影响

为确定工程中冷态条件下获得的推力室声学特性能否表征真实条件下的声学特性,研究了冷态无流动、热态气相流动和湍流两相燃烧三种状态下推力室声学振型及其阻尼特性。在推力室稳态流场中的有限区域施加数值定容弹,激发其具有多模态声学振型的大幅值压力振荡,采用衰减时间和半带宽来定量评价所激发的不同声学振型压力振荡衰减快慢,进而获得其阻尼特性。在相同过载比的数值定容弹激励下,在冷态条件下能激发包含更多声学振型压力振荡,且该振荡衰减时间更长,相同振型压力振荡衰减比热态条件下慢。在冷态条件下,一阶切向振型振幅最大,为最容易被激发声学振型;一阶纵向振型半带宽最小,为最难衰减的振型。在热态条件下,一阶纵向振型为最容易激发声学振型,也为最难衰减声学振型。从所激发的主要振型及其相对衰减的快慢来看,冷态条件下获得的声学特性能够表征真实条件下的推力室的声学特征。     

由太阳和地磁参数构成的信鸽导航原理仿真

根据信鸽导航理论和相关试验结果的分析,确定太阳高和地磁场参数的组合可以形成信鸽导航的环境基础.通过分析信鸽对太阳高度角、地磁倾角参数的可能利用过程,结合信鸽飞行路径的特点,确认了信鸽方向判断原理和逐渐趋紧的过程,并在此基础上,通过计算机程序对信鸽导航过程和分型线路进行了模拟,结果较为符合信鸽的飞行特点,并对信鸽导航的初步原理进行了分析和解释.     

地源热泵技术在建筑节能中的应用

本文探讨如何通过地源热泵技术实现建筑节能。研究通过地源热泵来实现一机多用,使其既能用于冬季供暖,又可以用于夏季制冷。同时也讨论了如何与太阳能相配合,来实现地热平衡。文中还给出了通过插值法和曲线拟合法对测量数据进行处理获得变温带和增温带的温度-深度曲线的方法。     

A Parallel Adaptive 3D MHD Scheme for Modeling Coronal and Solar Wind Plasma Flows

A parallel adaptive mesh refinement (AMR) scheme is described for solving the governing equations of ideal magnetohydrodynamics (MHD) in three space dimensions. This solution algorithm makes use of modern finite-volume numerical methodology to provide a combination of high solution accuracy and computational robustness. Efficient and scalable implementations of the method have been developed for massively parallel computer architectures and high performance achieved. Numerical results are discussed for a simplified model of the initiation and evolution of coronal mass ejections (CMEs) in the inner heliosphere. The results demonstrate the potential of this numerical tool for enhancing our understanding of coronal and solar wind plasma processes. This revised version was published online in June 2006 with corrections to the Cover Date.     

UVCS/SOHO Observations of Spectral Line Profiles in Polar Coronal Holes

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI.     

Composition Variations in the Solar Corona and Solar Wind

Order of magnitude variations in relative elemental abundances are observed in the solar corona and solar wind. The instruments aboard SOHO make it possible to explore these variations in detail to determine whether they arise near the solar surface or higher in the corona. A substantial enhancement of low First Ionization Potential (FIP) elements relative to high FIP elements is often seen in both the corona and the solar wind, and that must arise in the chromosphere. Several theoretical models have been put forward to account for the FIP effect, but as yet even the basic physical mechanism responsible remains an open question. Evidence for gravitational settling is also found at larger heights in quiescent streamers. The question is why the heavier elements don't settle out completely. This revised version was published online in June 2006 with corrections to the Cover Date.     

现代飞机俯仰跟踪时诱发振荡预测分析

根据飞机纵向ＰＩＯ的特点，提出了预测分析ＰＩＯ所用的人－机闭环系统数学模型，其中飞机采用等效系统数学模型，驾驶员操纵采用ＭｃＲｕｅｒ模型，参数按地面人－机模拟飞行跟踪试验确定，集中介绍了四种飞机纵向ＰＩＯ预测准则，Ｓｍｉｔｈ－Ｇｅｄｄｅｓ准则，修正带宽准则，增益，相位裕度准则，Ｎｅａｌ－Ｓｍｉｔｈ原则，并提供了相应的计算方法。     

驾驶员诱发振荡的抑制方法

对电传操纵系统驾驶员诱发振荡（ＰＩＯ）的现象进行了分析，指出了舵回路速率饱和是造成ＰＩＯ的主要原因，并有针对对给出了一种非常规的用于解决饱和非线性问题的程序控制方法。这种方法主要是通过舵回路反馈的状态信息来改变驾驶杆输入信号的放大系数，从而达到有效抑制ＰＩＯ的目的，同时用Ｈｕｒｗｉｔｚ稳定判据进行了机理分析，最后给出了仿真验证结果，证明该方法是简单而有效的。