影响Al2O3凝相尺寸分布的因素

用激光全息装置测量含铝复合推进剂燃烧场凝聚相的分布，分辨率为5μm。分析了滞留时间、铝粉含量（2％－16％）和燃烧室压强（0.1MPa-4MPa）对凝相粒子尺寸分布的影响，实验表明，粒子总数随滞留时间减少，粒子越大，减少的相对比例越大；粒子尺寸分布不随燃烧室压强和推进剂铝粉含量变化。     

影响Al2O3凝相尺寸分布的因素

用激光全息装置测量含铝复合推进剂燃烧场凝聚相的尺寸分布，分辨率为5μm。分析了滞留时间、铝粉含量(2%～16%)和燃烧室压强(0.1MPa～4MPa)对凝相粒子尺寸分布的影响。实验表明，粒子总数随滞留时间减少，粒子越大,减少的相对比例越大；粒子尺寸分布不随燃烧室压强和推进剂铝粉含量变化。     

基于数字同轴全息的铝颗粒燃烧粒度分布研究

铝颗粒的团聚效应会对固体推进剂燃烧造成不良影响,产生积渣、两相流损失等问题。为掌握铝颗粒的团聚机理,了解初始铝颗粒尺寸以及压强对铝团聚的影响,以优化推进剂配方及粒度级配,有必要对三维空间内铝颗粒的粒度分布进行研究。为解决传统检测方法的景深问题,采用了数字同轴全息（DIH）技术,并用普通镜头搭配4f透镜组取代长焦显微镜头构建了成像系统。实验一方面对两种具有不同初始粒径的推进剂A和B进行燃烧测量,另一方面对推进剂B分别在0.1,0.2,0.3MPa三种不同压强下的燃烧进行了测量,然后通过全息重建以及图像处理技术得到了燃烧铝颗粒的粒径信息,相对测量误差在9%以内,最后采用Normal和Log-Normal多峰拟合获取了粒度分布的详细参数。对比实验结果发现,常压下铝团聚体的尺寸随着初始铝粉粒径减小而减小;随着压强增大,铝团聚物的尺寸逐渐变小,体积概率密度逐步由双峰分布变为单峰分布,说明压强升高对于铝团聚有抑制作用。     

推进剂中铝凝聚——燃烧的影响因素初探

本文对含铝复合推进剂中影响铝的凝聚-燃烧的重要因素-AP粒度与铝粒度-进行了探讨.结果表明,两者对铝的凝聚-燃烧过程都有很大的影响.仅凝聚程度的大小而言,AP粒度的影响是主要的,而铝粉粒度的影响是第二位的;但对燃烧完全性来说,则需综合考虑     

在加速场下含铝复合推进剂燃烧中粒子动力学研究

从两个方面研究了在加速度场下含铝复合推进剂燃烧中粒子动力学：在理论分析中,以牛顿运动定律为基础,运用粘流Ｎ－Ｓ方程导出燃烧产物中凝聚铝粒子运动方程,计算出加速度与粒子临界尺寸的关系曲线;在试验研究中,用研制的燃烧实验装置和动态粒子采集器,在不同加速度条件下获取燃烧产物中的铝粒子。研究结果表明,理论分析计算和试验研究结果基本吻合,从而验证了加速度效应的基本原理。     

固体推进剂速度耦合响应函数测量实验方法研究

为获得固体推进剂速度耦合响应特性,基于T型燃烧器测量技术,建立了一种测量含铝复合推进剂速度耦合响应函数的实验方法,并在工作压强为6.5MPa和振荡频率约为175Hz条件下,开展了响应特性实验研究。实验结果表明:速度耦合与压强耦合有明显的不同,压强耦合在整个振荡区域内均表现出增益作用,而速度耦合在不同振荡区域内可表现出增益作用,也可以表现出抑制作用;在本文的工况参数条件下,速度耦合响应函数值远大于压强耦合响应函数值。在固体火箭发动机非线性燃烧不稳定中,速度耦合响应是不可忽略的重要影响因素。本文所建立的实验方法能在测量速度耦合响应函数的同时获得压强耦合响应函数,可更好地分析固体推进剂的燃烧响应特性。因此,该方法为分析固体火箭发动机非线性燃烧不稳定问题提供了重要的实验手段。     

含铝金属化浆体推进剂火箭发动机燃烧性能试验研究

为研究含铝浆体推进剂的燃烧特性,对浆体推进剂模型火箭发动机开展了一系列试验研究。分别将质量分数为21%的纳米铝粉颗粒以及质量分数为12%的氢化铝复合粒子加入到JP-10燃料中,对比分析了浆体燃料与纯净燃料在燃烧性能方面的差异。燃烧试验的氧燃比为1.6~2.0。试验结果表明:与纯净JP-10燃料相比,加入金属颗粒的JP-10浆体燃料在雾化和燃烧过程中产生了严重的结块聚集效应,导致其燃烧效率与质量比冲明显降低,而由于浆体燃料密度远大于纯净JP-10燃料,含纳米铝颗粒的浆体燃料的密度比冲相比于纯净JP-10燃料有大幅提高,提高幅度为5.5%~14.6%。试验还发现浆体燃料的点火延迟略低于纯净JP-10燃料,金属颗粒的加入对推进剂点火性能有积极的影响。试验中采集了喷管出口的固体燃烧产物并进行了XRD,EDS,SEM,TEM等多种手段分析,发现浆体燃料中铝的氧化率约为64%~74%,颗粒团聚现象明显,主要呈球形,尺寸分布不均,约为500nm~3μm。     

复合推进剂中铝粉凝聚的链反应模型

本文提出了描述复合火箭推进剂(HTPB/Ap/AL)体系中铝粉凝聚的新模型——链反应模型。定义并推导出了铝粉的凝聚速率、平均凝聚程度及铝凝滴直径大小分布函数的具体表达式,从中可明显看到推进剂燃速、铝粉含量与铝粉粒度,Ap粒度及燃烧室压力等因素对铝粉凝聚程度的影响趋势,并且与现有的实验结果完全相符。     

收集处理方法对含铝固体推进剂凝相燃烧产物特性影响

含铝固体推进剂凝相燃烧产物特性对固体火箭发动机的燃烧效率、燃烧稳定性和绝热安全性等影响重大。为获得准确可靠的凝相燃烧产物的理化特性,利用定压燃烧装置来收集凝相燃烧产物,采用马尔文激光粒度分析仪、扫描电镜及X射线衍射仪对产物进行表征,研究收集介质、干燥处理和超声分散对凝相燃烧产物性质的影响。结果表明,使用水收集获得的凝相燃烧产物平均粒度与氮气收集条件下相比大60%,水收集法适用于研究推进剂近燃面凝相燃烧产物。干燥处理能保证凝相燃烧产物样品中大尺寸颗粒的有效取样,在粒度测试之前需要对样品进行干燥处理来获取准确的凝相燃烧产物粒度分布数据。超声分散会导致大颗粒团聚物含量降低,小颗粒团聚物含量升高,最终显著降低凝相燃烧产物平均粒径。粒度测试时,在80kHz条件下,超声分散参数设定为40 W,5 min较为合适。基于研究结果,提出了一套科学合理的凝相燃烧产物收集处理方法。     

固体火箭喷管排气中的粒子分布

1.前言 现代的固体火箭发动机为提高推进剂的能量特性及抑制不稳定燃烧，常常在推进剂中添加金属粉末，最常见的是加金属铝粉。在发动机工作时，铝粉燃烧形成凝聚相的氧化铝粒子。这些粒子在喷管中的流动过程中，温度、速度等方面的变化滞后于燃·气本身的变     

Global Particle Simulation Study of Substorm Onset and Particle Acceleration

This paper reports the spatial and temporal development of Bursty Bulk Flows (BBFs) created by the reconnection as well as current disruptions (CDs) in the near-Earth tail using our 3D global EM particle simulation with a southward turning IMF in the context of the substorm onset. Recently, observations show that BBFs are often accompanied by current disruptions for triggering substorms. We haver examined the dynamics of BBFs and CDs in order to understand the timing and triggering mechanism of substorms. As the solar wind with the southward IMF advances over the Earth, the near-Earth tail thins and the sheet current intensifies. Before the peak of the current density becomes maximum, the reconnection takes place, which ejects particles from the reconnection region. Because of the earthward flows the peak of the current density moves toward the Earth. The characteristics of the earthward flows depend on the ions and electrons. Electrons flow back into the inflow region (the center of reconnection region), which provides current closure. Therefore the structure of electron flows near the reconnection region is rather complicated. In contrast, the ion earthward flows are generated far from the reconnection region. These earthward flows pile up near the Earth. The ions mainly drift toward the duskside. The electrons are diverted toward the duskside. Due to the pile-up, dawnward current is generated near the Earth. This dawnward current dissipates rapidly with the sheet current because of the opposite current direction, which coincides with the dipolarization in the near-Earth tail. At this time the wedge current may be created in our simulation model. This simulation study shows the sequence of the substorm dynamics in the near-Earth tail, which is similar to the features obtained by the multisatellite observations. The identification of the timing and mechanism of triggering substorm onset requires further studies in conjunction with observations.     

Energetic Particle Observations

The characteristics of solar energetic particles (SEP) as observed in interplanetary space provide fundamental information about the origin of these particles, and the acceleration and propagation processes at the Sun and in interplanetary space. Furthermore, energetic particles provide information on the development and structure of coronal mass ejections as they propagate from the solar corona into the interplanetary medium. In this paper we review the measurements of energetic particles in interplanetary space and discuss their implication for our understanding of the sources, and of acceleration and propagation processes.     

Particle Acceleration Mechanisms

In this paper we review the possible mechanisms for production of non-thermal electrons which are responsible for the observed non-thermal radiation in clusters of galaxies. Our primary focus is on non-thermal Bremsstrahlung and inverse Compton scattering, that produce hard X-ray emission. We first give a brief review of acceleration mechanisms and point out that in most astrophysical situations, and in particular for the intracluster medium, shocks, turbulence and plasma waves play a crucial role. We also outline how the effects of the turbulence can be accounted for. Using a generic model for turbulence and acceleration, we then consider two scenarios for production of non-thermal radiation. The first is motivated by the possibility that hard X-ray emission is due to non-thermal Bremsstrahlung by nonrelativistic particles and attempts to produce non-thermal tails by accelerating the electrons from the background plasma with an initial Maxwellian distribution. For acceleration rates smaller than the Coulomb energy loss rate, the effect of energising the plasma is to primarily heat the plasma with little sign of a distinct non-thermal tail. Such tails are discernible only for acceleration rates comparable or larger than the Coulomb loss rate. However, these tails are accompanied by significant heating and they are present for a short time of <10⁶ years, which is also the time that the tail will be thermalised. A longer period of acceleration at such rates will result in a runaway situation with most particles being accelerated to very high energies. These more exact treatments confirm the difficulty with this model, first pointed out by Petrosian (Astrophys. J. 557:560, 2001). Such non-thermal tails, even if possible, can only explain the hard X-ray but not the radio emission which needs GeV or higher energy electrons. For these and for production of hard X-rays by the inverse Compton model, we need the second scenario where there is injection and subsequent acceleration of relativistic electrons. It is shown that a steady state situation, for example arising from secondary electrons produced from cosmic ray proton scattering by background protons, will most likely lead to flatter than required electron spectra or it requires a short escape time of the electrons from the cluster. An episodic injection of relativistic electrons, presumably from galaxies or AGN, and/or episodic generation of turbulence and shocks by mergers can result in an electron spectrum consistent with observations but for only a short period of less than one billion years.     

Corotating Particle Events

The corotating particle events give us a unique opportunity to probe the three-dimensional structures of the heliosphere. This is especially true if we have observations over a period of extreme stability of the CIRs, such as existed over the recent solar minimum. We discuss how the observations fit into the context of current heliospheric magnetic field models. The energetic particle signatures of CIRs throughout the regions of the heliosphere covered by the deep-space missions are reviewed. The CIRs accelerate these particles and at the same time modulate both the high energy galactic cosmic rays and the anomalous cosmic rays.     

颗粒增强金属基复合材料凝固过程中的颗粒推移效应

归纳了颗粒增强金属基复合材料凝固过程中颗粒推移效应的各判据,分析了各自的适用范围,提出了实际复合材料铸件中抑制颗粒推移的途径。     

一种用于解决粒子滤波粒子退化现象的重要性重采样算法的研究

粒子滤波通过蒙特卡罗模拟来实现递推贝叶斯估计,在非线性非高斯系统中体现出良好的特性;但粒子滤波存在粒子退化现象的缺陷,针对这一问题,提出一种新的重采样算法,即分区重采样算法,其主要思想是根据多项式重采样与分层重采样算法的特点,把随机数区间划分成若干个区,每个区内的随机数任意排列,而区与区之间按升序排列。与目前常用的其他重采样算法相比,该方法提高了粒子滤波的平均性能,仿真实验验证了该算法的有效性和实用性。     

复合固体推进剂颗粒脱湿损伤参数反演

为确定复合固体推进剂颗粒脱湿损伤参数,采用分子动力学方法建立了复合固体推进剂颗粒夹杂模型,根据Surface-based cohesive方法,在高氯酸铵(AP)颗粒与基体之间的界面处设置接触损伤,对复合固体推进剂的细观损伤过程进行数值仿真计算。将数值仿真得到的应力-应变曲线与试验曲线进行对比,建立颗粒脱湿损伤参数的优化目标函数,通过分步迭代计算,对颗粒脱湿损伤参数进行反演识别。结果表明:根据反演参数计算复合固体推进剂细观损伤过程,颗粒夹杂模型表现出的宏观应力-应变关系与试验结果吻合良好,说明双折线损伤模型可以近似表征复合固体推进剂的脱湿损伤。     

Particle Acceleration in Relativistic Outflows

In this review we confront the current theoretical understanding of particle acceleration at relativistic outflows with recent observational results on various source classes thought to involve such outflows, e.g. gamma-ray bursts, active galactic nuclei, and pulsar wind nebulae. We highlight the possible contributions of these sources to ultra-high-energy cosmic rays.     

Particle Scattering by Magnetic Fields

The need for a correct quantitative treatment of the interactions between cosmic rays and turbulent magnetic fields continues to be one of the fundamental problems of modern astrophysics. It is the aim of this paper to review new developments in the understanding of mechanisms involved in the scattering of charged particles by magnetic field fluctuations. Special emphasis is given to a comparison of transport parameters determined from the modeling of spacecraft and neutron monitor observation of solar particle events, with theoretical predictions derived from a spectral analysis of simultaneously measured fluctuation spectra. It appears that the traditional quasi-linear theory of particle scattering requires only a slight modification, and the major problem still is our lack of knowledge of the three-dimensional structure of the magnetic turbulence. Possibilities to better reconcile the theory with observations by properly taking into account the microphysics of wave and turbulence aspects of the fluctuations, and to use energetic particles as probes to study certain properties of the magnetic turbulence, are discussed. This revised version was published online in August 2006 with corrections to the Cover Date.     

Relativistic Reconnection and Particle Acceleration

This chapter mainly deals with magnetic reconnection and particle acceleration in relativistic astrophysical plasmas, where the temperature of the current sheet exceeds the rest mass energy and the Alfvén velocity is close to the speed of light. Magnetic reconnection now receives a great deal of interest for its role in many astrophysical systems such as pulsars, magnetars, galaxy clusters, and active galactic nucleus jets. We review recent advances that emphasize the roles of reconnection in high-energy astrophysical phenomena.