冲击试验条件的转换方法及其应用

对冲击试验条件的转换方法进行了研究。利用从频域响应谱到时域激励信号的不唯一性,由小波合成法构造足够数量满足响应谱试验规范的时域激励信号,并施加到单机的有限元模型。用MSC．NASTRAN软件仿真计算单机中元器件安装位置处的响应。统计响应样本,获得在一定概率条件下元器件可能出现的响应峰值。将该峰值作为元器件冲击试验的半正弦波幅值,并以元器件产生最大响应的激励持续时间作为元器件冲击试验的作用时间参数,实现冲击试验条件的转换。给出了一个单机模型的冲击试验条件转换实例。     

High-speed unsteady flows past two-body configurations

This paper presents a detailed investigation of unsteady supersonic flows around a typical two-body configuration, which consists of a capsule and a canopy. The cases with different trailing distances between the capsule and canopy are simulated. The objective of this study is to examine the detailed effects of trailing distance on the flow fields and analyze the flow physics of the different flow modes around the parachute-like two-body model. The computational results show unsteady pulsating flow fields in the small trailing distance cases and are in reasonable agreement with the experimental data. As the trailing distance increases, this unsteady flow mode takes different forms along with the wake/shock and shock/shock interactions, and then gradually fades away and transits to oscillate mode, which is very different from the former. As the trailing distance keeps increasing, only the capsule wake/canopy shock interaction is present in the flow field around the two-body model, which reveals that the unsteady capsule shock/canopy shock interaction is a key mechanism for the pulsation mode.     

Suppressing unsteady motion of shock wave by high-frequency plasma synthetic jet

Three Plasma Synthetic Jet Actuators (PSJA) under the high-frequency actuation are used to control the Shock Wave Boundary Layer Interaction (SWBLI), a high-speed schlieren image processing method based on spatial Fourier transform as well as snapshot proper orthogonal decomposition were used to study the control effect of high-frequency plasma synthetic jet on low-frequency unsteadiness of SWBLI. The analysis of the base flow shows that the separated shock wave actually has both large- and small-amplitude vibrations at low frequency. And the results revealed that the PSJA with an operating frequency of 2 kHz has the ability to reduce the energy of low-frequency component of shock wave motion, indicating that the 2 kHz actuation can effectively suppress low-frequency unsteadiness of the separated wave. Compared with the actuation frequency of 2 kHz, the energy of low-frequency component of the shock wave is enhanced under the 8 kHz actuation, which aggravates the low-frequency unsteady motion of the shock wave. It is likely that the actuation frequency is too high, thus the intensity of the precursor shock wave induced by PSJA becomes weaker. Additionally, as the 4 kHz actuation is applied, the pulsation of the separation region was enhanced, it is speculated that the actuation frequency is coupled with the oscillation frequency of the separation region.     

激光─多普勒弹射冲击加速度校准方法

介绍了采用激光─多普勒偏振于涉系统绝对复现大位移、宽脉冲的冲击加速度量值的方法,说明了干涉系统的构成及原理。这种方法适合于长距离干涉测量和动态干涉测量。     

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。     

Experimental characteristics of oblique shock train upstream propagation

The structure and dynamics of an oblique shock train in a duct model are investigated experimentally in a hypersonic wind tunnel. Measurements of the pressure distribution in front of and across the oblique shock train have been taken and the dynamics of upstream propagation of the oblique shock train have been analyzed from the synchronized schlieren imaging with the dynamic pressure measurements. The formation and propagation of the oblique shock train are ini-tiated by the throttling device at the downstream end of the duct model. Multiple reflected shocks, expansion fans and separated flow bubbles exist in the unthrottled flow, causing three adverse-pressure-gradient phases and three favorable-pressure-gradient phases upstream the oblique shock train. The leading edge of the oblique shock train propagates upstream, and translates to be asym-metric with the increase of backpressure. The upstream propagation rate of the oblique shock train increases rapidly when the leading edge of the oblique shock train encounters the separation bubble near the shock reflection point and the adverse-pressure-gradient phase, while the oblique shock train slow movement when the leading edge of the oblique shock train is in the favorable-pressure-gradient phase for unthrottled flow. The asymmetric flow pattern and oscillatory nature of the oblique shock train are observed throughout the whole upstream propagation process.     

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。     

The onset of sunspot cycle 24 and galactic cosmic ray modulation

The annual mean sunspot number (SSN) has a minimum value in 2008, while the monthly mean SSN has a value of zero in August 2009. The galactic cosmic ray modulation for cycle 24 began at earth orbit in January 2010. We study the onset characteristics of the new modulation cycle using data from the global network of neutron monitors. They respond to time variations in different segments of the galactic cosmic ray rigidity spectrum. The corresponding temporal variations in the interplanetary magnetic field intensity (B) and solar wind velocity (V) as well as the tilt angle of the heliospheric current sheet are also studied. There is a lag of 3 months between a large, sharp increase of the tilt angle of the heliospheric current sheet and the onset of modulation. Some neutron monitors are undergoing long-term drifts of unknown origin.     

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.      

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.