推进剂用热塑性聚酯聚氨酯弹性体的结构与性能

针对推进剂粘合剂的需要,以聚己二酸乙二醇丙二醇酯(PEPA)为软段,异佛尔酮二异氰酸酯和1,4 丁二醇为硬段合成了一类能为硝酸酯增塑的热塑性聚氨酯弹性体(TPUE)。该弹性体采用熔融预聚法制备。利用GPC、FTIR、DSC、X Ray,力学性能测试和硝化甘油吸收实验等分析技术对聚合物的结构和性能进行了研究。结果表明,合成的热塑性聚氨酯弹性体具有较高的相对分子质量和聚氨酯的结构特征,具有较低的软段玻璃化转变温度和加工温度,具有较好的力学性能,以及与硝酸酯良好的相溶性,具有满足推进剂使用要求的力学性能。     

含能材料技术的进展与展望

对高能氧化剂、合能粘合剂、高能燃料等合能材料技术的进展分别作了扼要地阐述，介绍了含能材料技术领域的新概念和新技术，如多氮化合物(N5^ )、纳米材料(Alex)和低温固体推进剂(CSP)；对新型合能材料的应用及性能进行了综合比较与讨论。展望了含能材料技术的发展趋势。     

Relative fluxes of shock and prompt peaks in SEP event time profiles

Peak fluxes are an important property of gradual solar energetic particle (SEP) event time profiles from both astro/heliophysical and applications perspectives. However, the peak flux in an event may occur at the event onset, or at the time of the interplanetary shock arrival (the ESP or energetic storm particles). This makes an important difference in the interpretation of the peak flux, and in any attempts to characterize or model it. This paper describes a study of SEP data sets from ACE, IMP-8 and GOES toward determining the relative properties of these peak fluxes for protons with energies near 1, 10, and 50 MeV. The results suggest that for gradual events with both peaks, the ESP peak often dominates at 1 MeV energies and is dominant about half the time at 10 MeV. Moreover, the prompt peak fluxes can be used to estimate the shock peak (ESP event) up to days ahead, especially in the lower energy range.     

Properties of solar X-ray flares and proton event forecasting

X-ray flares and acceleration processes are in one complex of sporadic solar events (together with CMEs, radio bursts, magnetic field dissipation and reconnection). This supposes the connection (if not physical, but at least statistical) between characteristics of the solar energetic proton events and flares. The statistical analysis indicates that probability and magnitude of the near-Earth proton enhancement depends heavily on the flare importance and their heliolongitude. These relations may be used for elaboration of the forecasting models, which allow us to calculate probability of the solar proton events from the X-ray observations.     

5,5′-二硝基-3,3′-偶氮基-1-氢-1,2,4-三唑（DNAT）的合成和性能研究

以3,5-二氨基-1,2,4-三唑为原料,经过重氮化、选择性还原、酸性氧化3步,合成出目标化合物5,5′-二硝基-3,3′-偶氮基-1-氢-1,2,4三唑(DNAT),通过红外光谱、元素分析、质谱分析进行了结构鉴定,并进行了DSC-TGA、燃烧性能分析、感度测试等性能研究。实验结果表明,5,5′-二硝基-3,3′-偶氮基-1-氢-1,2,4-三唑(DNAT)化合物具有密度高(1.88 g/cm3)、正的生成焓(446.448 kJ/mol)、热稳定性能好的特点,是一种性能良好的高氮含能化合物。     

聚氨酯推进剂化学交联网络模型及c的计算

所谓复杂化学文联型聚氨酯网络是指固化体系中含有官能度大于4的预聚物及固化剂固化形成的交联网络。本文研究分析了复杂化学文联型聚氨酯（PU）网络形成过程和网络结构的特点，建立了复杂网络结构的简化模型，提出了计算其的理论公式。这些公式在PU弹性体及PU推进剂结构与性能之间关系的研究和PU泡沫、弹性体、PU固体推进剂等制品的质量控制中，将有广泛的应用。     

高能液体推进剂研究现状和应用前景

高能液体推进剂的发展有四个方面：金属化凝胶推进剂、高密度吸热型碳氢燃料推进剂、纳米材料液体推进剂、添加含能材料的液体推进剂。本文围绕高能液体推进剂的发展方向,综合论述了国内外的研究现状和应用前景分析,并提出了我国技术发展的初步思路。     

一步法制备BAMO-THF型热塑性弹性体及其力学特性

以一缩二乙二醇(DEG)为扩链剂,通过一步熔融聚合法,制备得到高含量3,3-二叠氮甲基氧丁环与四氢呋喃共聚醚(BAMO-THF)型含能热塑性弹性体(ETPE)。采用傅里叶变换红外光谱(FT-IR)和广角X-射线衍射仪(WXRD)表征制备的ETPE结构,动态力学热分析(DMA)、万能材料试验机、邵氏硬度仪研究其力学性质。结果表明,制备的BAMO-THF型ETPE具有明显的叠氮型聚醚聚氨酯弹性体特征。在加载应力和温度作用下,由于其线性分子链结构,ETPE试样蠕变程度较大。此外,扩链剂含量的增加并不利于ETPE延伸率和低温性能的提高。其中软段BAMO-THF含量达到93.3%,硬段含量仅为6.7%的D20试样力学性能较佳,抗拉强度和断裂伸长率分别为3.61 MPa和1 277%,低温玻璃化转变温度为-23.4℃。     

近月空间带电粒子环境——“嫦娥1号”“嫦娥2号”观测结果

“嫦娥1号”（CE-1）、“嫦娥2号”（CE-2）都安装了1台太阳高能粒子探测器（High-energetic ParticlesDetectors,HPD）和2台太阳风离子探测器（Solar Wind Ion Detectors,SWIDs）,进行了月球轨道200 km和100 km空间环境探测,获得了月球轨道空间高能带电粒子（质子、电子和重离子）能谱随时间的演化特征、等离子体与月球相互作用特征以及太阳风离子速度、密度和温度参量。空间环境探测数据分析结果表明：太阳活动低年、空间环境扰动水平相对较低、月球处于太阳风中时,近月空间带电粒子环境的基本特征与行星际空间相比变化不大。CE-1、CE-2在轨运行期间,发现了多起0.1～2 MeV能量电子急剧增加事件,这些事件发生在月球从太阳风运动到磁尾的所有空间区域,其中20%的事件伴随着卫星周围等离子体离子加速。模拟和统计研究表明：能量电子急剧增加使得绕月卫星和月球表面电位大幅下降导致了离子加速现象的发生;能量电子总流量大于10¹¹ cm^-2时,绕月卫星和月球表面充电电位可达负的上千伏。此外,月表溅射与反射太阳风离子、太阳风“拾起”离子等空间环境事件的发现,揭示了太阳风离子和月球存在复杂的相互作用过程。     

Solar proton events recorded in the stratosphere during cosmic ray balloon observations in 1957–2008

Long-term balloon observations have been performed by the Lebedev Physical Institute since 1957 up to the present time. The observations are taken several times a week at the polar and mid latitudes and allow us to study dynamics of galactic and solar cosmic ray as well as secondary particle fluxes in the atmosphere and in the near-Earth space. Solar energetic particles (120) – mostly protons – (SEP) events with >100 MeV proton intensity above 1 cm⁻² s⁻¹ s⁻¹ were recorded during 1958–2006. Before the advent of the SEP monitoring on spacecraft these results constituted the only homogeneous series of >100 MeV SEP events. The SEP intensities and energy spectra inferred from the Lebedev Physical Institute observations are consistent with the results taken in the adjacent energy intervals by the spacecraft and neutron monitors. Joint consideration of the SEP events series recorded by balloons and by neutron monitors during solar cycles 20–23 makes it possible to restore the probable number of events in solar cycle 19, which was not properly covered by observations. Some correlation was found between duration of SEP event production in a solar cycle and sunspot cycle characteristics.