模型发动机内凝相颗粒碰撞的数值模拟

针对燃烧室内的高温液态凝相粒子,利用所建立的数学模型对聚集状态下粒子间的碰撞与聚合及其与发动机壳体之间的相互作用过程开展了数值分析,获得了收敛管内壁面上液膜厚度及从出口处逃逸的粒子直径分布,并和实验数据进行了比较分析。结果表明在发动机两相内流场计算中,将凝相粒子看成无蒸发的液滴更为合适;聚集状态下凝相粒子间的碰撞与聚合对粒子直径的分布有很大的影响;粒子和壁面之间的相互碰撞不但会导致大量小尺寸粒子的生成,而且也是收敛管内壁面上金属膜形成的直接原因。     

挤压成型对LC4CS铝合金棒材阳极氧化膜结构的影响

研究了挤压成型对LC4CS铝合金棒材表面阳极氧化膜微观结构的影响。采用金相显微（OM）技术、扫描电镜（SEM）和能谱分析（EDS）等方法分析了铝合金基体中合金相的种类和分布、组织结构的变化规律以及阳极氧化膜的表面及断面形貌。研究发现,试样表面阳极氧化膜的结构特征与基体组织特征具有一致性。基体中的阳极相和阴极相颗粒分别导致了氧化膜中孔洞和夹杂缺陷的产生,在挤压变形中形成的析出相带以及不完全再结晶组织是造成氧化膜中凹坑结构和复杂网纹结构的主要原因。     

探测快中子的新技术(一)

概述了近年探则快中子的新技术，它们分别是：抑制γ射线、热中子和带电粒子的符合谱仪；高分辨、宽能量范围（0．1～15．0MeV）带正比计数器的3He夹心谱仪；含氢的纤维闪烁作用于抑制γ射线、中子位置分布和中子能谱测量，及合锂的纤维玻璃闪烁体用于长中子计数器测平均中子能量；中子的直接探测；用于中高能和重离子核物理的多元件阵列快中子探测器和极化仪；用于核核查的中子源影像探测器；高入射氚核能量和高能中子的伴随粒子技术等七个方面。它们对中子计量学的发展是重要的。     

Compression Creep Behavior of High Volume Fraction of SiC Particles Reinforced Al Composite Fabricated by Pressureless Infiltration

The compression creep deformation of the high volume fraction of SiC particles reinforced Al-Mg-Si composite fabricated by pressure-less infiltration was investigated. The experimental results show that the creep stress exponents are very high at temperatures of 673 K, 723 K and 773 K, and if taking the threshold stress into account, the true stress exponent of minimum creep strain rate is still approximately 5, although the volume fraction of reinforcements is very high. The creep strain rate in the high volume fraction rein- forced aluminum alloy matrix composites is controlled by matrix lattice diffusion. It is found that the creep-strengthening effect of high volume fraction of silicon carbide particles is significant, although the particles do not form effective obstacles to dislocation motion.     

Research on Feature Extraction of Remnant Particles of Aerospace Relays

The existence of remnant particles, which significantly reduce the reliability of relays, is a serious problem for aerospace relays. The traditional method for detecting remnant particles—particle impact noise detection (PIND)—can be used merely to detect the existence of the particle; it is not able to provide any information about the particles’ material. However, information on the material of the particles is very helpful for analyzing the causes of remnants. By analyzing the output acoustic signals from a PIND tester, this paper proposes three feature extraction methods: unit energy average pulse durative time, shape parameter of signal power spectral density (PSD), and pulse linear predictive coding coefficient sequence. These methods allow identified remnants to be classified into four categories based on their material. Furthermore, we prove the validity of this new method by processing PIND signals from actual tests.     

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.     

SEP events and multi-spacecraft observations: Constraints on theory

Fifteen solar energetic particle (SEP) events have been analyzed using proton flux data recorded by the Helios 1, Helios 2, and IMP 8 spacecraft in the energy range ∼4–40 MeV during 1974–1982. For each of the events at least two of the spacecraft have their nominal magnetic footpoint within 20° in heliocentric longitude from each other. The SEP events are sub-grouped as a function of their heliocentric longitudinal separation and heliocentric radial distance from the SEP associated solar flare and several case studies are presented in this paper. Main results concerning their usage in estimating the SEP radial dependence are given. Moreover, we investigate the behavior of the third not connected spacecraft in order to study the dependence of the proton flux as a function of flare location. It is found that the contribution of the longitudinal gradient in determining variations in the SEP proton flux is particularly relevant for spacecraft having their magnetic connection footpoint separated from the flare between 30° and 50°.     

Model of energetic populations at Ganymede,implications for an orbiter

A model is developed to study the energetic particle populations in Ganymede’s magnetosphere. The main objective is to estimate to what extent the moon could protect an orbiter from radiations. Using Liouville’s theorem, the phase space density of particles coming from Jupiter’s magnetosphere is calculated at any point of Ganymede’s environment. Up to energies of ∼50–100 keV for ions and ∼10–20 MeV for electrons, Ganymede’s magnetic field appears to be able to form distinctive populations as loss-cones over the polar caps and radiation belts. At larger energies, these features are blurred by Larmor radius effects; the moon absorption simply creates a quasi-isotropic layer of ∼500 km thickness where the flux is reduced by ∼40–50%. The predictions are compared to Galileo measurements. In particular, we demonstrate the importance of the moon sweeping in reducing the flux over the polar caps. Interestingly, this can be accounted for by assuming that the particles bouncing between Jupiter and Ganymede are ideally scattered in pitch angle and permanently re-fill the loss-cone, which increases the precipitation on Ganymede’s polar cap. In overall, it is estimated that the radiation dose received by an orbiter of Ganymede will be reduced by more than 50–60% compared to the expected dose at Jupiter/Ganymede distance. This should have a positive impact on the design of a future orbiter of Ganymede.     

模拟月尘制备及其物理和力学性质研究

在地球上进行的大量与月尘力学性质和机械性质相关的试验研究中,通常采用模拟月尘代替真实月尘。本研究制备了一种适用于月球探测工程试验的模拟月尘,制备工序依次为原材料选取、颗粒粗加工、颗粒精加工、颗粒级配、颗粒混合及预处理。该模拟月尘的颗粒粒径分布、颗粒相对密度、干密度、孔隙比、内聚力和内摩擦角等物理和力学性能参数经分析与国外典型模拟月尘相关参数相近,证明其可应用于月球探测工程试验。     

Energetic neutral atom (ENA) and charged particle periodicities in Saturn’s magnetosphere

The Magnetospheric Imaging Instrument (MIMI) on the Cassini spacecraft has observed energetic neutral atoms (ENA) and charged particles at Saturn from mid-2004 to the present. The particles often but not always reveal striking periodic behavior that seems to depend on the type of particle and spacecraft location. When subjected to a Lomb periodogram analysis, energetic electrons (>150 keV) exhibited strong frequency peaks near 10.80 h (the nominal or “base” period of Saturn kilometric radiation) during 2006–2008, but essentially no periodicity during 2005. The electron periodograms also show pronounced “double” frequency peaks in 2007 and 2008. Energetic protons (3–26 keV) show strong peaks near the same period for 2005–2007, but none for 2008. Oxygen ions at the same energies display strong peaks for 2005 and 2006, but not for 2007 and 2008. By projecting the ENA images onto Saturn’s equatorial plane or onto a plane perpendicular to the equatorial plane and then summing the data in the appropriate dimension, “strip” images can be constructed from which a time history can be derived. These time histories of ENA emissions are also subjected to a Lomb periodogram analyses. The energetic hydrogen neutrals (20–50 keV) exhibited periodic behavior only during 2007, while energetic oxygen neutrals (64–144 keV) displayed a strong SKR-like period in 2005 and 2006 but not for 2007 or 2008. Some of this behavior may be due to changing spacecraft aspect relative to the ENA emissions, and some of it may be real. This periodic behavior may be consistent with a rotating anomaly that “flashes” brightly in the midnight-to-dawn sector once per 10.8 h, with the flash parameters depending on particle species and energy.