基于ARVM模型的液体火箭发动机试验台故障预测方法

针对液体火箭发动机试验台故障子样少,故障预测精度低,故障维修保障困难等问题,在分析标准RVM优缺点的基础之上,提出了一种自适应能力较强的故障预测模型——ARVM(Adaptive Relevance Vector Machine)。为测试该模型,以某型轨控发动机高空模拟试验台管路流量、燃烧室压力为输入参量对推力矢量进行了预测,预测结果表明,ARVM方法能够有效跟踪推力矢量参数的变化趋势,并且获得了较高的预测精度和模型稀疏性。该方法对于复杂系统的故障预测和维修保障具有一定的理论价值和工程应用意义。     

面向小型自主航天器的锥-杆式对接机构锥面构型设计

对接锥是对接机构的重要组成部分,在碰撞过程中首先与主动对接机构相接触.比较小的锥角会造成系统在碰撞过程中发生剧烈振动,而比较大的锥角又会使系统的接触碰撞力增大,甚至造成对接失败.本文针对面向在轨服务的小型航天器上使用的锥——杆式对接机构,提出了新的对接锥型面设计目标;利用有限元分析软件ANSYS/LS-DYNA,仿真分析了对接机构碰撞后的运动学特性;通过研究对接锥的型面设计方法,得到了新型对接锥型面.研究结果表明,新型对接机构的整体性能满足设计目标要求.     

固体火箭发动机喷管摆角校准方法研究

介绍了固体火箭发动机全轴摆动喷管的摆角校准技术方法,论述了为实现该技术而采取的技术措施以及新结构、新方法的建立过程。以FG-xx发动机喷管摆角校准数据证明了该技术的适用性和高精度指标。     

液体火箭发动机性能参数的贝叶斯评估方法

文章研究了如何利用发动机地面试验数据,来评估飞行中的性能参数及其可靠性。采用贝叶斯分析,研究给出了合理实用的先验分布及后验分布的求解,并给出了各参数及其性能可靠性的贝叶斯点估计和置信估计。     

基于过程神经网络的液体火箭发动机状态预测

提出一种基于极限学习算法的离散过程神经网络模型,用于解决液体火箭发动机状态预测这一难题。首先,在历史数据的基础上建立离散过程神经网络（DPNN）预测模型;然后,根据在线更新的数据样本,采用递推极限学习（EL）算法对双并联前馈离散过程神经网络（DPFDPNN）隐层到输出层的权值进行更新,并应用权值更新后的过程神经网络对发动机状态进行预测;最后,以液体火箭发动机状态预测中氢涡轮泵扬程预测为例,分别采用有权值更新和无权值更新两种预测模型进行了试验。结果表明,通过更新过程神经网络权值可以使模型具有更高的预测精度和更好的适应能力,该方法能够为液体火箭发动机状态预测提供一种有效的解决途径。      

固体火箭发动机羽焰测温方法研究

根据固体火箭发动机羽焰特征研制了多目标多光谱高温仪,它可同时测量羽焰六个目标点的温度,每个目标点均有八个工作波长。同时提出了求解真温的实用方法,完成了固体火箭发动机羽焰温度及其分布的测量。     

液体火箭发动机试验脉动压力数据分析方法研究

针对液体火箭发动机试验脉动压力数据的特点,对脉动压力数据和相关振动测点数据进行快速傅里叶变换(FFT),频谱分析的结果能够有效判断发动机不稳定燃烧的声振类型。采用小波变换奇异点检测的方法,对启动段和关机段波动异常的脉动压力数据进行分析,结合相关振动测点的频谱信息能够在时域内准确定位奇异点位置,提取频域内的信息,有效判断推进剂燃烧情况和声振类型。分析结果表明上述方法在火箭发动机和组合件试验的脉动压力数据分析中具有重要的推广意义。     

一种液体火箭发动机试验台螺纹拧紧力矩量化控制方法

针对液体火箭发动机试验台工艺装配可靠性提升的需求,提出一种螺纹拧紧力矩量化控制方法。利用非试验和试验环境的力矩值统计与分析,确定液体火箭发动机试验台螺纹拧紧力矩值区间;通过拧紧力矩强度理论计算,验证力矩值区间的合理性;结合试验台螺纹空间位置的具体特点,确定适用不同空间位置的力矩量化控制方法和流程,并在试验中进行了应用。应用结果表明,本文提出的方法可有效提高发动机试验工艺的可靠性。     

一种液体火箭发动机试验台螺纹拧紧力矩量化控制方法

针对液体火箭发动机试验台工艺装配可靠性提升的需求,提出一种螺纹拧紧力矩量化控制方法。利用非试验和试验环境的力矩值统计与分析,确定液体火箭发动机试验台螺纹拧紧力矩值区间;通过拧紧力矩强度理论计算,验证力矩值区间的合理性;结合试验台螺纹空间位置的具体特点,确定适用不同空间位置的力矩量化控制方法和流程,并在试验中进行了应用。应用结果表明,本文提出的方法可有效提高发动机试验工艺的可靠性。     

一种改进的固液火箭发动机故障诊断方法

针对固液火箭发动机的可靠性问题,设计了一种改进的贝叶斯网络故障诊断方法,可以通过网络化自主逻辑推理,对固液火箭发动机进行故障诊断。为了提取时序观测信号的故障特征,提出将步进法与核主成分分析(KPCA)相结合的分析方法,并根据模糊C均值聚类算法(FCM)建立模糊多态贝叶斯网络,实现对观测信号尺度的模糊处理,提高对不确定性故障的诊断能力。通过Matlab/Simulink建立改进的贝叶斯网络故障诊断系统。仿真结果表明,改进的算法能够实现对固液火箭发动机常见故障的有效诊断,并能够适应小样本集学习的情况。与传统贝叶斯诊断算法相比,故障诊断的平均准确率提高了20.9%。     

The parameters of shock acoustic waves generated during rocket launches

We investigate the form and dynamics of shock acoustic waves (SAW) generated during the launching of rockets Proton and Soyuz from the Baikonur cosmodrome in 1998–2000. In spite of the difference of geophysical conditions, the ionospheric response for all launchings had the character of an N-wave with a period of about 300 s and with an amplitude far exceeding background fluctuations. The angle of elevation of the SAW wave vector varies from 30° to 65°, and the SAW phase velocity (800–1200 m/s) approaches the sound velocity at heights of the ionospheric F region maximum. The position of the SAW source, inferred by neglecting refraction corrections, corresponds to the segment of the rocket path at a distance no less than 700–900 km from the launch pad, which is consistent with the estimated delay time of SAW source triggering (250–300 s).     

Magnetogasdynamic shock wave generated by a moving piston in a rotational axisymmetric isothermal flow of perfect gas with variable density

The propagation of a strong cylindrical shock wave in an ideal gas with azimuthal magnetic field, and with or without axisymmetric rotational effects, is investigated. The shock wave is driven out by a piston moving with time according to power law. The ambient medium is assumed to have radial, axial and azimuthal component of fluid velocities. The fluid velocities, the initial density and the initial magnetic field of the ambient medium are assumed to be varying and obey power laws. Solutions are obtained, when the flow between the shock and the piston is isothermal. The gas is assumed to have infinite electrical conductivity and the angular velocity of the ambient medium is assumed to be decreasing as the distance from the axis increases. It is expected that such an angular velocity may occur in the atmospheres of rotating planets and stars. The shock wave moves with variable velocity and the total energy of the wave is non-constant. The effects of variation of the initial density and the Alfven-Mach number on the flow-field are obtained. A comparison is also made between rotating and non-rotating cases.     

Solar atmosphere wave dynamics generated by solar global oscillating eigenmodes

The solar atmosphere exhibits a diverse range of wave phenomena, where one of the earliest discovered was the five-minute global acoustic oscillation, also referred to as the p-mode. The analysis of wave propagation in the solar atmosphere may be used as a diagnostic tool to estimate accurately the physical characteristics of the Sun’s atmospheric layers.In this paper, we investigate the dynamics and upward propagation of waves which are generated by the solar global eigenmodes. We report on a series of hydrodynamic simulations of a realistically stratified model of the solar atmosphere representing its lower region from the photosphere to low corona. With the objective of modelling atmospheric perturbations, propagating from the photosphere into the chromosphere, transition region and low corona, generated by the photospheric global oscillations the simulations use photospheric drivers mimicking the solar p-modes. The drivers are spatially structured harmonics across the computational box parallel to the solar surface. The drivers perturb the atmosphere at 0.5?Mm above the bottom boundary of the model and are placed coincident with the location of the temperature minimum. A combination of the VALIIIC and McWhirter solar atmospheres are used as the background equilibrium model.We report how synthetic photospheric oscillations may manifest in a magnetic field free model of the quiet Sun. To carry out the simulations, we employed the magnetohydrodynamics code, SMAUG (Sheffield MHD Accelerated Using GPUs).Our results show that the amount of energy propagating into the solar atmosphere is consistent with a model of solar global oscillations described by Taroyan and Erdélyi (2008) using the Klein-Gordon equation. The computed results indicate a power law which is compared to observations reported by Ireland et al. (2015) using data from the Solar Dynamics Observatory/Atmospheric Imaging Assembly.     

Spatio-temporal structure of the wave packets generated by the solar terminator

Using long-term (1998--2009) total electron content (TEC) measurements from the GPS global network including dense network of GPS sites in USA and Japan, we have obtained the first data regarding the spatio-temporal structure and the statistics of medium-scale traveling wave packets (MS TWPs) excited by the solar terminator (ST). Total amount of the detected TWPs exceeds 565,000. There is no correlation between TWPs occurrence and geomagnetic and solar activity. We found that the diurnal, seasonal and spectral MS TWPs characteristics are specified by the solar terminator (ST) dynamics. MS TWPs are the chains of narrow-band TEC oscillations with single packet’s duration of about 1–2 h and oscillation periods of 10–20 min. The total duration of chain is about 4–6 h. The MS TWPs spatial structure is characterized by a high degree of anisotropy and coherence at the distance of more than 10 wavelengths. Occurrence rate of daytime MS TWPs is high in winter and during equinoxes. Occurrence rate of nighttime MS TWPs has its peak in summer. These features are consistent with previous MS travelling ionosphere disturbance (TID) statistics obtained from 630-nm airglow imaging observations in Japan. In winter, MS TWPs in the northern hemisphere are observed 3–4 h after the morning ST passage. In summer, MS TWPs are detected 1.5–2 h before the evening ST appearance at the point of observations, but at the moment of the evening ST passage in the magneto-conjugate point. The obtained results are the first experimental evidence for the hypothesis of the ST-generated ion sound waves.     

基于CE/SE法的翼型流场激波捕捉计算

在二维四边形结构网格下,针对时空守恒元和解元(CE/SE, space-time Conservation Element and Solution Element)方法捕捉激波需要双倍空间网格点的问题,重新对守恒元和解元进行了定义,计算点同时包含单元中心和网格节点,并推导得到了新的CE/SE方法的计算公式.以此为基础,结合非敏感克朗数(CNIS, Courant Number Insensitive Scheme)计算格式和当地时间步长方法,对激波翼型流场进行数值模拟,并与原方法及AGARD报告进行对比.结果表明,对原CE/SE方法的改进是有效的,可明显提高激波分辨能力,并且激波前后无明显的数值震荡发生,新方法适合应用于翼型流场中捕捉激波.     

Dependence of ESP intensity on collisionless shock wave characteristics

Flux variations of 1 – 5 MeV protons are studied in energetic storm particle events with respect to the preshock solar wind plasma parameters and to the thickness of the collisionless interplanetary shock wave. It is found that the peak intensity in ESP events depends on pre-shock plasma density and on the thickness of the transition region. These relations predict, in agreement with recent observations, the increase of ESP events at larger heliocentric distances.     

Plasma wave signatures of collisionless shocks and the role of plasma wave turbulence in shock formation

We review observations of the plasma waves associated with collisionless shocks, and summarize our understanding of their generation mechanisms and importance to shock physics. The emphasis is on waves generated directly at the shock, especially ion acoustic and lower-hybrid-like modes. The observations are discussed in the context of shock structure, with attention to the distinctions between waves generated in the shock foot and ramp. The behavior of resistive, dispersive and supercritical quasiperpendicular shocks is contrasted. Evidence for the operation of various generation mechanisms, including interactions with cross field currents, gyrating reflected ions and field aligned electron beams, are summarized. The various forms of plasma heating which are actually observed are then outlined and the role of the various wave modes in this heating is discussed. We argue in conclusion that, while plasma wave turbulence may play a vital role in plasma heating for some special shocks, it is of second order importance in most cases.     

用GAO-YONG湍流模型计算激波/边界层干扰

采用GAO-YONG可压缩湍流方程组,模拟了平板激波/湍流边界层干扰现象.运用SIMPLE算法求解方程组,并分别采用三阶精度的QUICK格式和中心格式离散对流项和扩散项.计算结果较好预测了入射斜激波在平直壁面引起湍流附面层分离的流动特征: 分离点的反射激波、分离包引起的膨胀扇以及再附点的反射激波.对流场的时均参数与实验值进行了比较,计算得到的壁面压力分布、摩阻系数分布和速度型与实验值比较吻合很好.结果表明GAO-YONG可压缩湍流方程组能够高精度模拟平板激波/湍流边界层干扰流动.      

Indication of convectively generated gravity waves observed by CLAES

Cryogenic Limb Array Etalon Spectrometer temperature data are analyzed for gravity waves (GWs) using the same methods previously employed for CRISTA data. We obtain nearly 1.5 years of continuous GW data between 34°S and 34°N and good coverage at higher latitudes depending on UARS yaw maneuvers. Correlations of GW variances with sea surface temperature indicate strong convective forcing above the Gulf of Mexico and the Kuro-Shio stream as well as above source regions in the southern subtropics during the summer months of the respective hemisphere. However, it appears difficult to clearly separate between convective forcing and the effects of the background winds, for which similar correlations are found. Further progress in accessing GW sources therefore can be expected mainly from improved measurements, which could provide also information about the GW horizontal wavelength as well as from quantitative comparisons to model predictions.     

空间激光干涉引力波探测器轨道修正方法

针对空间激光干涉引力波探测器轨道修正问题,提出一种基于虚拟编队构型设计的航天器轨道修正方法。空间激光干涉引力波探测器由3颗航天器组成等边三角形构型。由于入轨误差和摄动的影响,探测器的构型不稳定。假设名义轨道上运行着一颗理想航天器,实际轨道上的真实航天器与之组成虚拟编队,探测器的3颗真实航天器分别与对应的理想航天器组成3个虚拟编队。考虑探测器构型稳定性要求和摄动的影响,对虚拟编队的构型进行设计,进而求解航天器平均轨道要素修正量。求解得到的航天器平均轨道要素修正量小于偏差量,轨道修正通过四脉冲控制实现。数值仿真结果表明,该方法通过部分轨道修正满足了探测器的构型稳定性要求,具有减少燃料消耗、延长任务寿命的潜力。