几种主要陨石类型的Hugoniot参数

根据各类陨石的模式化学组成或矿物组成,采用比容叠加法计算了铁陨石,ＥＨ和ＥＬ群顽辉石球粒陨石,Ｈ,Ｌ和ＬＬ群普通球粒陨石这几种主要陨石类型的Ｈｕｇｏｎｉｏｔ参数,计算结果与已表的同灰型陨石的冲击波压缩数据一致。     

侧面安装使用的压力传感器用激波管进行动态特性校准的方法研究

通过理论分析和实验结果指出了用激波管动压校准装置校准压力传感器时被校传感器安装在激波管侧面进行校准存在的问题 ,给出了如何对侧面安装使用的压力传感器用激波管进行动态特性校准的方法。     

机匣转静刮磨后轴流压气机气动性能评估研究

为揭示机匣可磨耗涂层磨损造成的叶尖间隙和粗糙度变化对压气机气动性能的影响规律,针对不同刮磨形貌下Rotor 37转子性能进行了数值模拟研究。结果表明,压气机等熵效率和出口流量对刮磨间隙和粗糙度的变化较为敏感,降幅最高可达1.78%和0.83%,而压比变化不大;刮磨间隙深度增加,刮磨最深位置前移时,叶尖泄漏增强,泄漏流与上端壁附面层及主流相互作用演变为泄漏涡,与激波相互干涉,造成较大的叶尖损失;压气机气动性能受磨损区域粗糙度影响较小,虽然等熵效率对粗糙度变化较为敏感,但最大降幅也仅为0.38%。磨损区域粗糙度增加时,近壁区湍流波动加强且气流更易分离,引起叶尖泄漏流和叶片尾迹区域的流动结构变化,使压气机气动特性向低流量方向偏移。     

高能电弧等离子体激励控制双压缩拐角激波/边界层干扰实验研究

超声速/高超声速飞行器进气道入口处多采用多级压缩构型,其诱导的激波/边界层干扰严重影响进气道效率和飞行器的气动性能,因此对双压缩拐角激波/边界层干扰进行流动控制具有较强的应用背景。在来流速度为Ma=2.0的风洞内,针对三种典型的双压缩拐角构型,开展了高能流向脉冲电弧放电阵列调控双压缩拐角激波/边界层干扰的实验研究,并对激励流场的高速纹影图像进行了空间梯度阈值处理和均方根处理。结果显示,在激励的作用下两道分离激波的强度均减弱,验证了利用高能流向脉冲电弧放电阵列控制双压缩拐角激波/边界层干扰的可行性。在分析控制效果的基础上,获得了在不同构型拐角的流场中前驱冲击波列和控制气泡的演化规律,结合控制效果的时序特征,最终揭示了高能流向脉冲电弧放电阵列作用于双压缩拐角激波/边界层干扰的前驱控制和接续控制的接力控制机理。     

一种新的飞行器运输振动负荷确定方法浅探

指出了飞行器实物运输试验面临的问题，提出了采用等比模型实物进行运输试验的方法。通过对该方法的基本原理及关注重点予以阐释，在充分运用试验数据的基础上，对提高飞行器运输状态下抗振动冲击设计能力提出建议。     

Magnetospheric electric field variations caused by storm-time shock fronts

On January 20, 2005 there was an X 7.1 solar flare at 0636 UT with an accompanied halo coronal mass ejection (CME). The resultant interplanetary shock impacted earth ∼36 h later. Near earth, the Advanced Composition Explorer (ACE) spacecraft observed two impulses with a staircase structure in density and pressure. The estimated earth-arrival times of these impulses were 1713 UT and 1845 UT on January 21, 2005. Three MINIature Spectrometer (MINIS) balloons were aloft on January 21st; one in the northern polar stratosphere and two in the southern polar stratosphere. MeV relativistic electron precipitation (REP) observed by all three balloons is coincident (<3 min) with the impulse arrivals and magnetospheric compression observed by both GOES 10 and 12. Balloon electric field data from the southern hemisphere show no signs of the impulse electric field directly reaching the ionosphere. Enhancement of the balloon-observed convection electric field by as much as 40 mV/m in less than 20 min during this time period is consistent with typical substorm growth. Precipitation-induced ionospheric conductivity enhancements are suggested to be (a) the result of both shock arrival and substorm activity and (b) the cause of rapid (<6 min) decreases in the observed electric field (by as much as 40 mV/m). There is poor agreement between peak cross polar cap potential in the northern hemisphere calculated from Super Dual Auroral Radar Network (SuperDARN) echoes and horizontal electric field at the MINIS balloon locations in the southern hemisphere. Possible reasons for this poor agreement include (a) a true lack of north–south conjugacy between measurement sites, (b) an invalid comparison between global (SuperDARN radar) and local (MINIS balloon) measurements and/or (c) radar absorption resulting from precipitation-induced D-region ionosphere density enhancements.     

动力学环境质量载荷效应的统计能量分析与试验研究

对质量载荷在冲击、振动及噪声等动力学环境上的影响作了统计能量分析（ＳＥＡ）与试验研究。分析与试验结果是满意的,其结论对工程系统动力学环境预示、评估和制定试验条件有重要意义。     

考虑间隙非线性的控制舵非线性气动弹性分析

间隙结构的气动弹性系统非线性颤振问题是飞行器气动弹性力学工程领域的研究热点和难点,研究 考虑间隙非线性的控制舵系统的气动弹性特性具有重要意义。基于最小状态拟合方法获得时域降阶气动力模 型,并通过Lagrange方程获得系统非线性气动弹性方程;对比分析三种不同非线性控制舵系统的极限环颤振 及非线性动力学响应特性,并与等效线化法和时域仿真的结果进行一致性对比。结果表明:俯仰和扑动弹簧刚 度的变化对系统颤振边界有显著影响,当俯仰和扑动两个方向同时含有间隙非线性时,系统在线性颤振速度内 存在倍周期、混沌等复杂非线性动力学现象。     

运用一维太阳风MHD CE/SE模型预报行星际激波到达时间

在一维太阳风磁流体(MHD)数值模拟中, 应用时空守恒元和解元(Conservation Element/Solution Element, CE/SE)方法, 建立了一个行星际激波扰动传播模型(1D-MHD (CE/SE)模型), 用来预报行星际激波到达时间. 收集了1997年2月至2002年8月间的137个激波事件, 对激波到达地球轨道附近的传播时间进行了预测, 并将预报结果与STOA, ISPM, HAFv.2以及SPM模型所得结果进行比较. 对于相同的样本事件, 1D-MHD (CE/SE)模型给出的渡越时间平均绝对值误差并不大于其他4个模型, 且该模型预报的相对误差小于10 %的事件占25.6 %, 小于30 %的事件占69.3 %, 小于50 %的事件占87.6 %, 其预报精度与其他模型相比基本相当. 这表明该模型在空间天气的激波到达时间预报方面有潜在的应用价值.      

Cosmological Shock Waves

Large-scale structure formation, accretion and merging processes, AGN activity produce cosmological gas shocks. The shocks convert a fraction of the energy of gravitationally accelerated flows to internal energy of the gas. Being the main gas-heating agent, cosmological shocks could amplify magnetic fields and accelerate energetic particles via the multi-fluid plasma relaxation processes. We first discuss the basic properties of standard single-fluid shocks. Cosmological plasma shocks are expected to be collisionless. We then review the plasma processes responsible for the microscopic structure of collisionless shocks. A tiny fraction of the particles crossing the shock is injected into the non-thermal energetic component that could get a substantial part of the ram pressure power dissipated at the shock. The energetic particles penetrate deep into the shock upstream producing an extended shock precursor. Scaling relations for postshock ion temperature and entropy as functions of shock velocity in strong collisionless multi-fluid shocks are discussed. We show that the multi-fluid nature of collisionless shocks results in excessive gas compression, energetic particle acceleration, precursor gas heating, magnetic field amplification and non-thermal emission. Multi-fluid shocks provide a reduced gas entropy production and could also modify the observable thermodynamic scaling relations for clusters of galaxies.