密封舱内漂浮小球运动规律的数值模拟研究

"天宫二号"空间实验室开展了首次人机协同在轨维修技术试验,机械臂操作终端抓取漂浮小球试验为在轨试验任务之一。为研究漂浮小球与机械臂操作终端运动特性之间的匹配性,文章建立了在轨微重力环境下小球运动的物理模型与数学模型,采用动网格方法对不同小球的运动特性进行数值模拟,得到小球的运动规律,由此确定小球的设计参数范围,作为机械臂操作终端系统方案设计的依据。最终,数值模拟结果与"天宫二号"空间实验室在轨试验数据的对比初步验证了该计算结果的正确性。     

一种气动式冲击响应谱试验系统的设计与分析

大多数航天器单机产品都要求进行冲击响应谱试验,试验量级普遍为1000g~2000g,甚至超过3000g。对于较大质量(如50 kg以上)产品高量级的冲击试验,振动台、传统的摆锤式或跌落式冲击试验台均很难满足相关要求。文章研究并设计了一套能够进行大质量受试产品高量级冲击响应谱试验的气动冲击试验系统。该系统利用压缩空气瞬间释放膨胀推动质量块加速撞击具有多阶固有频率的谐振板,通过谐振板被激起的响应模拟复杂的衰减正弦波。测试结果表明,系统空载时冲击谱量级达8000g,负载200 kg时可达5000g,时域曲线为振荡衰减波,持续时间小于10 ms。文章提出的气动式冲击响应谱试验系统设计方法可为此类冲击试验系统的设计提供参考和理论依据。     

超额定状态下二元超声速进气道的流动特性

为了揭示超额定工作状态下超声速进气道内的复杂流动机理,对一设计马赫数为2.0的二元超声速进气道开展了数值模拟研究,获得了其在不同来流马赫数状态、不同节流状态下的流场结构.结果表明:当进气道工作在额定状态时,随着节流程度的增加,其激波串的核心区由偏向下壁面摆至偏向上壁面;而在超额定状态下,由于依次受到唇罩内侧分离包、唇罩激波等的影响,激波串核心区则由偏向上壁面转而摆至偏向下壁面.在来流马赫数为2.5的节流状态下,其唇罩激波与前体斜激波相交形成了马赫杆等复杂波系结构,而来流马赫数为3.0状态却并未形成此类现象.在上述两种超额定工作状态下,前体斜激波的上透射激波均在高反压条件下演化为正激波形态,而唇罩激波的下透射激波形态也发生了明显的改变.      

一种正向乘波前体设计方法初步研究

以定楔角乘波体设计方法为基础,研究了影响高超/超声速乘波体"乘波"的主要因素,给出了前体前缘实际气流压缩角的确定方法及影响因素,可知在相同的来流马赫数和压缩角δ下,随着前缘角θ和气流与前缘夹角α的增加,实际气流偏转角γ减小。据此,基于幂函数进气道前体构形,给出了前缘激波不脱体的限制条件及具体的判定方法,分析了乘波体典型几何特征参数对前缘激波不脱体的影响规律,结果显示在相同的来流马赫数和压缩角度下,增大前缘形状因子n,减小前体的长宽比L/W及增大前缘角均有利于激波不脱体。根据给出的前体几何参数对前缘激波脱体的影响规律曲线,对一种"前体几何外形构造+前缘激波附体条件限制"的正向前体乘波器工程设计方法进行了研究,给出了具体设计流程,并进行了初步的数值仿真验证,表明通过该方法设计的乘波前体流动特征与预期的结果吻合,说明文中所给出的激波附体条件及影响规律是可信的,乘波前体设计方法是可行的。     

超声速气流与反向射流的混合

在不同的反向射流喷射角度条件下,对反向射流混合加热方案的混合效果进行了实验研究。采用空气和氢气燃烧混合物作为超声速载气流,常温下的空气作为反向射流。将混合前后流场的温度分布作为衡量载气流与反向射流混合效果的标志。实验结果表明:混合均匀度随混合距离的增加而提高;反向射流的喷射角度在40°角附近时混合均匀度最佳;增大反向射流初始压力可有效提高反向射流与载气流的流量比,从而提高混合效率。     

Structure and kinetic properties of slow-mode shocks associated with magnetic reconnection in the near-Earth magnetotail

We study the structure and kinetic properties of slow-mode shocks near the plasma sheet boundary layer (PSBL) associated with magnetic reconnection by Cluster observation. The presence of slow-mode shocks is confirmed by traditional Rankine–Hugoniot (RH) analysis and Monte-Carlo shock fitting method. The Walén analysis, applied to the tailward flow associated with slow-mode shocks, also supports that plasma was accelerated across a Petschek-type slow-mode shock connected to the diffusion region. Back-streaming ions were observed on the shock layer, and cold ions were accelerated and heated by slow-mode shocks. In addition, whistler and electrostatic solitary waves were observed around the slow-mode shocks. These waves might be excited by the observed field-aligned electron beams near the shocks.     

斜激波极值规律的边界层影响

采用边界层理论与斜激波/膨胀波精确算法，建立一种结合Eckert参考温度法和Illingworth-Stewartson变换法优势的边界层权重算法，用于研究超声速黏性楔面边界层位移厚度对斜激波极值规律的影响。分别应用层流Navier-Stokes方程和湍流Navier-Stokes方程的CFD解算器对边界层新模型进行了算例精度评估。在来流马赫数为1.2~2.4和楔面角为3°~20°的范围内，压强比的相对误差小于0.1%。计入层流与湍流边界层影响的理论模型研究表明，边界层影响使得最优马赫数增加；对于层流边界层，最优马赫数增量约为0.001 5~0.003 3；对于湍流边界层，最优马赫数增量约为0.002 8~0.006 1。     

Geomagnetic activity associated with magnetic clouds,magnetic cloud-like structures and interplanetary shocks for the period 1995–2003

Using nine years (1995–2003) of solar wind plasma and magnetic field data, solar sunspot number, and geomagnetic activity data, we investigated the geomagnetic activity associated with magnetic clouds (MCs), magnetic cloud-like structures (MCLs), and interplanetary shock waves. Eighty-two MCs and one hundred and twenty-two MCLs were identified by using solar wind and magnetic field data from the WIND mission, and two hundred and sixty-one interplanetary shocks were identified over the period of 1995–2003 in the vicinity of Earth. It is found that MCs are typically more geoeffective than MCLs or interplanetary shocks. The occurrence frequency of MCs is not well correlated with sunspot number. By contrast, both occurrence frequency of MCLs and sudden storm commencements (SSCs) are well correlated with sunspot number.     

Propagation and interaction of interplanetary transient disturbances. Numerical simulations

We study the heliocentric evolution of ICME-like disturbances and their associated transient forward shocks (TFSs) propagating in the interplanetary (IP) medium comparing the solutions of a hydrodynamic (HD) and magnetohydrodynamic (MHD) models using the ZEUS-3D code [Stone, J.M., Norman, M.L., 1992. Zeus-2d: a radiation magnetohydrodynamics code for astrophysical flows in two space dimensions. i – the hydrodynamic algorithms and tests. Astrophysical Journal Supplement Series 80, 753–790]. The simulations show that when a fast ICME and its associated IP shock propagate in the inner heliosphere they have an initial phase of about quasi-constant propagation speed (small deceleration) followed, after a critical distance (deflection point), by an exponential deceleration. By combining white light coronograph and interplanetary scintillation (IPS) measurements of ICMEs propagating within 1 AU [Manoharan, P.K., 2005. Evolution of coronal mass ejections in the inner heliosphere: a study using white-light and scintillation images. Solar Physics 235 (1–2), 345–368], such a critical distance and deceleration has already been inferred observationally. In addition, we also address the interaction between two ICME-like disturbances: a fast ICME 2 overtaking a previously launched slower ICME 1. After interaction, the leading ICME 1 accelerates and the tracking ICME 2 decelerates and both ICMEs tend to arrive at 1 AU having similar speeds. The 2-D HD and MHD models show similar qualitative results for the evolution and interaction of these disturbances in the IP medium.     

Interplanetary Physics Research in China:2006—2008

This brief report summarized the latest advances of the interplanetary physics research in China during the period of 2006—2007,made independently by Chinese space physicists and through international collaboration.The report covers all aspects of the interplanetary physics,including theoretical studies,numerical simulation and data analysis.