磁尾中性片与磁尾正交曲线坐标系

根据磁尾中性计随地磁倾角变化的特点用光滑函数拟合中性片曲面模式,并用ISEE卫星的磁场资料来确定曲面参数。本中性片模式既保持了中性片的基本变化特征,又可以在近地处光滑过渡到赤道面。在此基础上,建立了一个以中性片曲面为坐标面的磁尾正交曲线坐标系。这个坐标系随地磁倾角的变化而变化,用这个坐标系可将不同的地磁倾角的磁场位形变换成地磁倾角为零时的标准形式,从而便于分析卫星的观测数据。      

新型中性聚合物键合剂设计与合成

首先以三-(2-甲基氮丙啶基)氧化膦(MAPO)与丙烯酸(AA)为原料合成MAPO的衍生物,通过红外和质谱对产物进行了定性分析,用非水滴定的方法检测氮丙啶环的含量,通过正交试验设计得到了较优工艺条件:MAPO与AA的摩尔比为1:1,反应温度为70 ℃,反应时间为2.5 h,所得氮丙啶环含量最接近理论值.再利用该活性中间体与丙烯腈、丙烯酸羟乙酯共聚,得到改性的中性聚合物键合剂,通过接触角的测量,粘接性能预估表明,该新型中性聚合物键合剂与黑索金(RDX)、奥克托金(HMX)、高氯酸铵(AP)的界面浸润好、粘接强.     

Ozone variability related to several SEP events occurring during solar cycle no. 23

Data from geostationary operational environmental satellite (GOES) series were used to identify intense solar energetic particle (SEP) events occurred during the solar activity cycle no. 23. We retrieved O₃, NO, NO₂, HNO₃, OH, HCl and OHCl profiles coming from different satellite sensors (solar occultation and limb emission) and we looked for the mesospheric/stratospheric response to SEPs at high terrestrial latitudes. The chemistry of the minor atmospheric components is analysed to evaluate the associated odd nitrogen (NO_x) and odd hydrogen (HO_x) production, able to cause short (h) and medium (days) term ozone variations. We investigated the effects of SEPs on the polar atmosphere in three different seasons, i.e., January 2005, April 2002 and July 2000. The inter-hemispheric variability of the ozone, induced by the SEP series of January 2005, has been compared with the effects connected both to larger and quite similar events. We found that during SEP events: (i) solar illumination is the key factor driving SEP-induced effects on the chemistry of the polar atmosphere; (ii) even events with limited particle flux in the range 15–40 MeV are able to change the abundance of the minor constituents in the mesosphere and upper stratosphere.     

December 2006 solar extreme events and their influence on the near-Earth space environment: “Universitetskiy-Tatiana” satellite observations

The Russian microsatellite “Universitetskiy-Tatiana” was launched on Jan. 20, 2005 and was both a scientific and educational mission. Its two main aims were declared as: (1) monitoring of the energetic particles dynamics in the near-Earth space environment after solar events and during quiet times, (2) educational activities based on experimental data obtained from the spacecraft. In this paper observations acquired during Dec. 5–16, 2006, known as “Solar Extreme Events 2006”, were analyzed. The “Universitetskiy-Tatiana” microsatellite orbit permits one to measure both solar energetic particle dynamics, variations of the boundary of solar particle penetration, as well as relativistic and sub-relativistic electrons of the Earth’s outer radiation belt during and after magnetic storms. Both relativistic electrons of the Earth’s outer radiation and solar energetic particles are an important source of radiation damage in near-Earth space. Therefore, the presented experimental results demonstrate the successful application of a small educational spacecraft both for scientific and educational programs.     

Study of correlations between waves and particle fluxes measured on board the DEMETER satellite

The topic of relativistic electron dynamics in the outer radiation belt has received considerable attention for many years. Nevertheless, the problem of understanding the physical phenomenon involved is far from being resolved. In this paper, we use DEMETER observations to examine the variations of the energetic electron fluxes and ELF/VLF wave intensities in the inner magnetosphere during the intense 8 November 2004 magnetic storm. Electron flux spectra and associated wave intensity spectra are analysed throughout the magnetic storm and common characteristics or differences to other storm events are retained. The overall objective of this study is to identify and derive parameters that are relevant for particle flux modelling; the time constant characterizing the persistent decay after particle enhancement was found to be one of these important model parameters.The analysis of the 8 November 2004 event reveals that for L-shell parameter higher than 4, an electron flux dropout is observed during the storm’s main phase for electrons in the energy range 0.1–1 MeV, as has been reported from other measurements. Characteristic wave spectra accompanying this phase are analysed. They show a typical enhancement in the frequency range 0.3–10 kHz at onset for all L-shell values under consideration (2 < L < 5). During the first stage of the recovery phase, the electron fluxes are increased to a level higher than the pre-storm level, whereas the level of wave intensity in the frequency range observed below 300 Hz is at its highest. In the second stage, the particle flux decrease goes hand in hand with a global wave activity decline, the relaxation time of the latter being smaller than the former’s one. In some other cases, long-lasting electron enhancement associated with constant wave activity has been observed during this latter stage. For the above mentioned storm, while at low L values the decay time constants are higher for low energy electrons than for high energy electrons, this order is reversed at high L values. At about L = 3.6 the time constant is independent of electron energy.     

A new modeling method of solar energetic proton events for ISO specification

Solar energetic protons degrade performance and reliability of spacecraft systems due to single-event effects, total dose effects and displacement damage in electronics components including solar cells. On designing a solar cell panel, a total fluence of solar energetic protons (SEPs) which cause solar cell damage is needed to estimate power loss of the solar cells over mission life. Nowadays a solar panel area of spacecraft is increasing as spacecraft mission life becomes longer (15–18 years). Thus an accurate SEP model is strongly required for the cost-minimum design from the aerospace industry. The SEP model, JPL-91 proposed by Feynman et al., is currently used widely for solar cell designing. However, it is known that the JPL-91 model predicts higher fluences of protons than values actually experienced in space, especially after 7 years on orbit. In addition, the model is based on several assumptions, and also needs Monte-Carlo simulations for calculating fluences. In this study, we propose a new method for modeling SEPs especially focused on solar cell degradation. The newly-proposed method is empirical, which constructs a model based directly upon proton flux measurement data taken by instruments onboard spacecraft. This method has neither assumptions nor dependence on SEP event selection, both of which are needed in JPL-91. The model fluences derived from this method show lower fluences in longer missions compared to JPL-91. This method has been proposed to ISO (International Organization for Standardization) and has been discussed for a new standard SEP model.     

美国的中性浮力模拟器及其应用

中性浮力地面模拟试验不仅可以用来训练航天员,对大型空间结构的设计及在轨组装与维修技术研究也具有重要的作用.文章对美国的三台大型中性浮力模拟器的性能、规模和配置及几次典型的大型空间结构的中性浮力模拟试验作了介绍.     

太赫兹雷达前沿探测成像技术

综述几种典型的太赫兹雷达前沿探测成像技术。首先,回顾太赫兹雷达技术的发展历程,分析其实用化进程中面临的挑战;然后,分别从太赫兹雷达增程、前视成像探测以及雷达信号处理三个方面展开论述,梳理太赫兹单光子探测、里德堡原子探测、孔径编码成像、涡旋目标微动探测以及智能信息处理五种典型的太赫兹雷达探测前沿技术的研究背景、基本原理、技术优势等;最后,对全文进行总结。研究成果有望为突破太赫兹雷达在作用距离、探测体制等方面的技术瓶颈提供可行的技术途径,并进一步推动太赫兹探测机理、方法、器件和系统等全面创新发展,为战场侦察、精确打击以及远程预警等应用提供关键技术支撑。     

带筋整体壁板预应力喷丸成形数值模拟及变形预测

带筋整体壁板特别是高筋整体壁板具有优异的结构效率、减重效益和密封效果，在航空航天等领域备受青睐。预应力喷丸成形是大中型、长寿命、高性能复杂带筋整体壁板的一种不可多得的有效成形手段。数值模拟是促进带筋整体壁板预应力喷丸成形技术研究、进步与应用的一种极具潜力的途径。针对带筋整体壁板预应力喷丸成形数值模拟，建立了基于响应面函数的多弹丸撞击有限元模型、基于应变中性层内移的反弯曲应力场法模拟模型、预应力喷丸成形RBF神经网络预测模型，实现了喷丸成形应力场法数值模拟、预应力喷丸成形较高精度数值模拟与变形预测，为带筋整体壁板预应力喷丸成形技术研究和实际应用提供了一种更为便捷、高效、经济的途径。     

基于线性重力差模型的拦截弹中制导技术

针对机载动能拦截弹的中制导段气动力作用可忽略且存在无法实时精确计算重力偏差等特点，提出了一种基于线性重力差模型的预测制导方法。通过线性模型逼近中制导过程中拦截弹与目标之间的重力偏差，以此为依据调整拦截弹的推力矢量并将重力偏差值消除。在此基础上采用延迟点火的策略使得拦截弹的拦截器助推级更好地修正预测模型与实际情况的偏差，经过仿真验证可以将整个中制导段的脱靶量限制在一个较小数值，从而为末制导段提供良好的初始条件。