3,3'-二硝胺基-4,4'-偶氮呋咱二肼盐的合成、表征及性能研究

以二氨基呋咱(DAF)为原料,经氧化、硝化、中和反应合成出3,3'-二硝胺基-4,4'-偶氮呋咱二肼盐(Hy2DNAAF),对其结构进行了表征,并对其热性能、机械感度性能、爆轰性能、单元推进剂和Hy2DNAAF-CMDB推进剂的性能进行了研究。结果表明,Hy2DNAAF的热分解峰温为208℃,特性落高为25.7cm。Hy2DNAAF的理论爆速为8635m/s,理论爆压为32.61GPa,Hy2DNAAF单元推进剂的理论比冲为2717N·s/kg,特征速度为1734.3m/s。Hy2DNAAFCMDB推进剂的理论比冲为2 522.9N·s/kg,特征速度为1591.1m/s。     

GAP基含能聚氨酯弹性体包覆RDX的研究

为了以较小的能量损失获得低感度的包覆RDX,采用液相沉淀法,以GAP基含能聚氨酯弹性体对RDX进行了包覆研究。通过傅立叶红外光谱(FTIR)、扫描电镜(SEM)、X射线光电子能谱(XPS)、差示扫描量热法(DSC)、有机元素分析、感度测试、流散性测试等方法对包覆样品进行了表征。结果表明,包覆样品颗粒表面有明显包覆层存在,颗粒流散性较包覆前有所提高,包覆度R为72.5%,包覆层质量分数为0.98%,与投料值1%基本相当;热分解峰温较包覆前有所降低;包覆样品的FTIR谱图中在2 100 cm-1附近含有明显的—N3吸收峰,且峰形尖锐;以1%GAP基聚氨酯弹性体包覆的RDX的特性落高从包覆前的25.6 cm提高到47.9 cm,增加近1倍;摩擦感度爆炸百分数从72%下降到40%。     

超高速撞击下PTFE/Al含能材料薄板的载荷特性分析

不同于传统惰性材料的空间碎片防护结构,含能材料防护结构在超高速撞击下的冲击起爆特性是其防护能力得以提高的根本原因。PTFE/Al含能材料防护结构的冲击起爆特性改变了弹丸强冲击载荷下的破碎机制,弹丸内部的冲击压力对于分析含能材料在超高速撞击下的防护机理具有重要意义。对超高速撞击试验中回收的PTFE/Al防护结构后板进行损伤特性分析,获得了对应速度条件下弹丸的破碎特性。基于一维冲击波理论,分析PTFE/Al靶板在超高速撞击条件下的冲击响应过程,结合考虑化学反应效率的热化学反应模型,获得了弹丸在碰撞与爆炸联合作用下的载荷特性,通过与试验结果对比验证,获得该材料完全反应的临界撞击速度约为1800 m/s,弹丸的临界破碎速度为2875 m/s,小于铝防护结构中对应的临界破碎速度。给出了弹丸在PTFE/Al、铝两种防护结构中产生相同冲击压力时对应的临界速度,分别为弹道段的800 m/s和破碎段的3580 m/s。     

含能材料废料处理技术研究述评(Ⅰ)——安全销毁技术

概括了国内外固体推进剂、火炸药等含能材料(EM)废料处理技术的发展情况,介绍了缩小EM废料尺寸的高压液体切割技术和使EM废料脱敏的碱解法和乳化法等预处理技术,EM废料安全销毁的熔盐销毁(MSD)法、水热氧化(HTO)法、电化学法、湿空气氧化法等化学销毁技术以及堆肥合成、生物降解和生物转化的生物销毁技术。其中预处理与化学、生物处理相结合的综合销毁技术可以实现含能材料废料的安全销毁,最后分析了EM废料安全销毁技术研究的主要特点和发展趋势。     

高能电子辐照下介质-导体相间结构深层充电特性研究

为研究影响介质-导体相间结构深层充电特性的内在因素,设计了不同构型的试验样品,利用90Sr放射源模拟空间高能电子环境对样品进行深层充电辐照试验,测量了充电电位的差异。并借助深层充电三维仿真软件计算介质-导体相间结构在不同几何构型情况下的深层充电电位、电场分布。试验和仿真结果表明,介质最高表面电位以及介质内部最大电场均与介质宽度和高度呈正相关。其他条件不变时,介质越宽,或越高于导体表面,发生放电的风险就越高。在介质与导体侧面存在微小缝隙情况下,介质内最大电场显著增强,易发生内部击穿。而在介质与导体之间的真空间隙内,电场很容易超过击穿阈值,放电风险很大。航天工程应用中为降低此种结构深层充放电的风险,在满足绝缘性能及其他要求的前提下应尽量减小介质的宽度,降低介质与导体间的高度差,并确保介质与导体侧面接触良好。     

Viewing radiation signatures of solar energetic particles in interplanetary space

A current serious limitation on the studies of solar energetic particle (SEP) events is that their properties in the inner heliosphere are studied only through in situ spacecraft observations. Our understanding of spatial distributions and temporal variations of SEP events has come through statistical studies of many such events over several solar cycles. In contrast, flare SEPs in the solar corona can be imaged through their radiative and collisional interactions with solar fields and particles. We suggest that the heliospheric SEPs may also interact with heliospheric particles and fields to produce signatures which can be remotely observed and imaged. A challenge with any such candidate signature is to separate it from that of flare SEPs. The optimum case for imaging high-energy (E > 100 MeV) heliospheric protons may be the emission of π⁰-decay γ-rays following proton collisions with solar wind (SW) ions. In the case of E > 1 MeV electrons, gyrosynchrotron radio emission may be the most readily detectible remote signal. In both cases we may already have observed one or two such events. Another radiative signature from nonthermal particles may be resonant transition radiation, which has likely already been observed from solar flare electrons. We discuss energetic neutrons as another possible remote signature, but we rule out γ-ray line and 0.511 MeV positron annihilation emission as observable signatures of heliospheric energetic ions. We are already acquiring global signatures of large inner-heliospheric SW density features and of heliosheath interactions between the SW and interstellar neutral ions. By finding an appropriate observable signature of remote heliospheric SEPs, we could supplement the in situ observations with global maps of energetic SEP events to provide a comprehensive view of SEP events.     

The Seed Population for Energetic Particles Accelerated by CME-Driven Shocks

Understanding properties of solar energetic particle (SEP) events associated with coronal mass ejections has been identified as a key problem in solar-terrestrial physics. Although recent CME shock acceleration models are highly promising, detailed agreement between theoretical predictions and observations has remained elusive. Recent observations from ACE have shown substantial enrichments in the abundances of ³He and He⁺ ions which are extremely rare in the thermal solar wind plasma. Consequently, these ions act as tracers of their source material, i.e., ³He ions are flare suprathermals and He⁺ ions are interstellar pickup ions. The average heavy ion composition also exhibits unsystematic differences when compared with the solar wind values, but correlates significantly with the ambient suprathermal material abundances. Taken together these results provide compelling evidence that CME-driven shocks draw their source material from the ubiquitous but largely unexplored suprathermal tail rather than from the more abundant solar wind peak. However, the suprathermal energy regime has many more contributors and exhibits much larger variability than the solar wind, and as such needs to be investigated more thoroughly. Answers to fundamental new questions regarding the preferred injection of the suprathermal ions, the spatial and temporal dependence of the various sources, and the causes of their variability and their effects on the SEP properties are needed to improve agreement between the simulations and observations.     

Energetic Hydrogen and Oxygen Atoms Observed on the Nightside of Mars

We present measurements of energetic hydrogen and oxygen atoms (ENAs) on the nightside of Mars detected by the neutral particle detector (NPD) of ASPERA-3 on Mars Express. We focus on the observations for which the field-of-view of NPD was directed at the nightside of Mars or at the region around the limb, thus monitoring the flow of ENAs towards the nightside of the planet. We derive energy spectra and total fluxes, and have compiled maps of hydrogen ENA outflow. The hydrogen ENA intensities reach 10⁵ cm⁻² sr⁻¹ s⁻¹, but no oxygen ENA signals above the detection threshold of 10⁴ cm⁻² sr⁻¹ s⁻¹ are observed. These intensities are considerably lower than most theoretical predictions. We explain the discrepancy as due to an overestimation of the charge-exchange processes in the models for which too high an exospheric density was assumed. Recent UV limb emission measurements (Galli et al., this issue) point to a hydrogen exobase density of 10¹⁰ m⁻³ and a very hot hydrogen component, whereas the models were based on a hydrogen exobase density of 10¹² m⁻³ and a temperature of 200 K predicted by Krasnopolsky and Gladstone (1996). Finally, we estimate the global atmospheric loss rate of hydrogen and oxygen due to the production of ENAs.     

自主火星探测高集成离子与中性粒子分析仪

小型化、高集成化是深空探测载荷发展的主要趋势。在我国自主火星探测计划中,设计了一种高集成化的火星离子与中性粒子分析仪。采用从传感器到电子学进行最大限度共用的设计思路,在一台仪器中实现对离子和能量中性原子进行能量、方向和成分的探测,大大降低了仪器对卫星平台的资源需求。仪器采取静电分析进行离子的方向和能量测量、采取飞行时间方法进行离子成分的测量。中性原子采用电离板电离成带电离子,后端的能量测量和成分测量与离子相同。鉴定件样机已经完成了初步的测试定标,结果表明其满足设计要求。     

2 AU以内的“渐进型”太阳高能粒子事件模拟

太阳高能粒子（Solar Energetic Particle,SEP）事件是影响地球空间以及深空辐射环境的主要因素之一。“渐进型”太阳高能粒子事件中的高能粒子主要来自于日冕物质抛射（Coronal Mass Ejection,CME）所驱动的激波扩散加速（Diffusive Shock Acceleration,DSA）过程。CME驱动的激波在行星际的传播过程中,其结构不断演化,进而影响到高能粒子的加速过程。本文利用二维太阳高能粒子加速和传播模型,对发生于2014年4月18日的太阳高能粒子事件实例进行了数值模拟。模型考察了黄道面上2 AU的距离以内包含地球所在位置的4个不同点,分别计算了每个点上高能粒子的通量。数值模拟的结果表明：黄道面内不同位置的观察点,与激波波前的磁力线连接不同,从而导致观察点处高能粒子的通量有着显著的差异。该模型的计算结果可以为深空探测计划开展辐射环境研究提供必要的输入。