轮体结构颗粒阻尼器设计方法

利用离散元法及正交设计方法,对典型轮体结构发生伞形振动时的二维等效振动模型进行了空腔尺寸及颗粒填充方案的数值设计,并结合振动试验结果给出了轮体结构颗粒阻尼器的设计流程及设计准则.研究表明:1建立的二维等效振动模型在能够反映轮体结构伞形振动基本特征的同时,也可以较为准确地模拟内部颗粒运动对结构产生的影响;2颗粒阻尼对轮体结构的振动有明显的改善作用,但填充不同材质的颗粒,其减振效果会有较为明显的区别;3空腔的尺寸及颗粒的质量率对颗粒阻尼的影响显著,应首先保证的是较高的颗粒质量率;4由于碰撞间隙的作用,对于固定规格的空腔和颗粒,存在最佳颗粒体积填充率使得颗粒阻尼的减振效果最佳.由试验与数值模拟的最佳方案的一致性可知,发展的设计方法可以较为准确地给出轮体结构颗粒阻尼器的最优空腔尺寸及其对应的最佳填充方法,可用于轮体结构伞形振动减振方案的前期设计.     

一种基于NGA-QPF的航天器姿态估计方法

针对航天器姿态确定中的非线性非高斯的滤波问题,提出一种基于遗传算法的粒子滤波的航天器姿态估计方法。该方法将姿态四元数作为采样粒子进行粒子滤波,并将小生境遗传算法（NGA）引入粒子滤波算法中,以改善粒子滤波的性能;用遗传算法单独进行陀螺偏差估计,以减少粒子滤波的状态维数。该姿态估计方法保持了四元数的归一化性质,通过引入小生境遗传算法解决了重采样阶段的粒子退化问题,并且由于单独估计陀螺偏差避免了粒子滤波状态的扩展。该方法能够在较少粒子的情况下实现高效率高精度的定姿,仿真结果说明了方法的有效性。     

A summary of the applications of a weighted average method determining times of solar cycle extrema

This paper is a summary of our recent researches on the applications of a weighted average method determining times of solar cycle extrema in the prediction of solar activity. Some correlation coefficients among the parameters in solar cycle according to this definition are higher than those according to the conventional definition. The descending time is found to be correlated (r = −0.77) with the ascending time 3 cycles earlier. The amplitude of solar cycle is found to be correlated (r = −0.77) with the max–max solar cycle length 2 cycles earlier. The ascending time is found to be correlated (r = −0.72) with the amplitude. A newly defined parameter called effective duration is found to be well correlated (r = 0.86) with the amplitude 5 cycles later. These correlations suggest that earlier cycles should influence later ones. The next (24th) solar cycle is estimated to start in March 2007 ± 7 months, reach its maximum in January 2011 ± 14 months, with a size of 150 ± 22, larger than those from some correlations according to the conventional definition.     

传导发射测量不确定度评定的验证

为了保证测量不确定度评定结果有足够的可信度,必须对评定的测量不确定度进行验证。概述了采用蒙特卡洛模拟法验证传导发射测量不确定度的方法,介绍了通过埃奇沃思级数估计测量结果概率分布的过程和应用蒙特卡洛方法解决实际问题的基本步骤,最后结合某试验室的实例给出了验证结果,证明在大部分频点上其根据GUM评定的传导发射测量不确定度是可信的。     

基于联合滤波器的高精度卫星定姿系统设计

设计了由陀螺、GPS姿态敏感器、红外地平仪和太阳敏感器构成的太阳同步极轨卫星姿态确定系统。提出联邦滤波器结构和算法,推导了各子系统的量测方程和姿态确定系统的误差状态方程。为规避对量测值进行非相关处理,采用减小GPS姿态敏感器输出的姿态滤波值作为系统滤波器量测值的频率的方法。仿真结果表明,采用联邦滤波器对多敏感器卫星姿态确定系统进行信息融合,具有计算量小、精度高、可靠性好等优点。     

Equilibration Processes in the Warm-Hot Intergalactic Medium

The Warm-Hot Intergalactic Medium (WHIM) is thought to contribute about 40–50% to the baryonic budget at the present evolution stage of the universe. The observed large scale structure is likely to be due to gravitational growth of density fluctuations in the post-inflation era. The evolving cosmic web is governed by non-linear gravitational growth of the initially weak density fluctuations in the dark energy dominated cosmology. Non-linear structure formation, accretion and merging processes, star forming and AGN activity produce gas shocks in the WHIM. Shock waves are converting a fraction of the gravitation power to thermal and non-thermal emission of baryonic/leptonic matter. They provide the most likely way to power the luminous matter in the WHIM. The plasma shocks in the WHIM are expected to be collisionless. Collisionless shocks produce a highly non-equilibrium state with anisotropic temperatures and a large differences in ion and electron temperatures. We discuss the ion and electron heating by the collisionless shocks and then review the plasma processes responsible for the Coulomb equilibration and collisional ionisation equilibrium of oxygen ions in the WHIM. MHD-turbulence produced by the strong collisionless shocks could provide a sizeable non-thermal contribution to the observed Doppler parameter of the UV line spectra of the WHIM.     

Thermodynamical Properties of the ICM from Hydrodynamical Simulations

Modern hydrodynamical simulations offer nowadays a powerful means to trace the evolution of the X-ray properties of the intra-cluster medium (ICM) during the cosmological history of the hierarchical build up of galaxy clusters. In this paper we review the current status of these simulations and how their predictions fare in reproducing the most recent X-ray observations of clusters. After briefly discussing the shortcomings of the self-similar model, based on assuming that gravity only drives the evolution of the ICM, we discuss how the processes of gas cooling and non-gravitational heating are expected to bring model predictions into better agreement with observational data. We then present results from the hydrodynamical simulations, performed by different groups, and how they compare with observational data. As terms of comparison, we use X-ray scaling relations between mass, luminosity, temperature and pressure, as well as the profiles of temperature and entropy. The results of this comparison can be summarised as follows: (a) simulations, which include gas cooling, star formation and supernova feedback, are generally successful in reproducing the X-ray properties of the ICM outside the core regions; (b) simulations generally fail in reproducing the observed “cool core” structure, in that they have serious difficulties in regulating overcooling, thereby producing steep negative central temperature profiles. This discrepancy calls for the need of introducing other physical processes, such as energy feedback from active galactic nuclei, which should compensate the radiative losses of the gas with high density, low entropy and short cooling time, which is observed to reside in the innermost regions of galaxy clusters.     

Kuafu and the studies of CME initiation

We first briefly review the current trend in the studies of coronal mass ejections (CMEs), then summarize some recent efforts in understanding the CME initiation. Emphasis has been put on the studies of Earth-directed CMEs whose associated surface activity and large scale magnetic source have been well identified. The data analysis by combining the MDI full disc magnetograms, vector magnetograms of active regions, EUV waves and dimmings, non-thermal radio sources, and the SOHO LASCO observations has shed new light in understanding the CME magnetism. However, the current studies seem to invoke new observations in a few aspects: (1) The observations which enable us to trace CMEs from the earliest associated surface activity to its initial acceleration and key development in the low corona in the height of 1–3 R; (2) The imaging spectroscopic observations which can be used to diagnose the early plasma outflow and the line-of-sight velocity in understanding the kinematics of CMEs; (3) The accurate timing from primary magnetic energy release, manifested by chromospheric activity, non-thermal radio bursts, and EUV, X-ray and γ-ray emissions, to the CME initiation, early acceleration and propagation, and the consequences in the interplanetary space and magnetosphere. The Kuafu Mission will meet the basic requirement for the new observations in CME initiation studies and serve as a monitor of space weather of the Sun–Earth system.     

空间碎片撞击在轨感知技术研究综述

随着航天发射活动的日益频繁,空间碎片环境随之恶化。为了应对空间碎片的撞击威胁,人们提出了用空间碎片撞击在轨感知系统实时监测航天器在轨遭受空间碎片撞击的情况。文章在对国内外相关研究机构研究成果的调研基础上,介绍了国内外在空间碎片撞击在轨感知技术领域的研究现状,对各国基于超高速撞击声发射技术的空间碎片撞击在轨感知技术的发展状况进行了全面评述,重点介绍了国内的研究进展。最后基于国内航天事业需要,探讨了未来发展方向。     

碳纤维复合材料贮箱内压和低温承载行为研究

碳纤维增强聚合物复合材料具有轻质高强的优异特性,是液氢液氧燃料贮箱的理想材料。然而液氢液氧燃料贮箱在服役时要承受极低温度载荷,复合材料贮箱箱体的低温结构可靠性尚未可知。开展了碳纤维/环氧复合材料缠绕贮箱结构在温度和内压载荷下的变形及损伤研究,分别进行了常温/低温抗渗漏测试,结合应变测量、声发射监测、氦质谱检漏等方法分别研究了内压以及低温工况对复合材料贮箱的应变分布及损伤泄漏状态影响机制。研究结果表明,封头与圆筒区域交界处易产生应变集中,低温载荷导致复合材料局部小幅度基体损伤及纤维/基体界面脱粘,但并未影响贮箱箱体承压性能和气密性。本研究可为未来大型航天器减质设计提供参考。