Formation and Composition of Planetesimals

The composition of planetesimals depends upon the epoch and the location of their formation in the solar nebula. Meteorites produced in the hot inner nebula contain refractory compounds. Volatiles were present in icy planetesimals and cometesimals produced in the cold outer nebula. However, the mechanism responsible for their trapping is still controversial. We argue for a general scenario valid in all regions of the turbulent nebula where water condensed as a crystalline ice (Hersant et al., 2004). Volatiles were trapped in the form of clathrate hydrates in the continuously cooling nebula. The epoch of clathration of a given species depends upon the temperature and the pressure required for the stability of the clathrate hydrate. The efficiency of the mechanism depends upon the local amount of ice available. This scenario is the only one so far which proposes a quantitative interpretation of the non detection of N₂ in several comets of the Oort cloud (Iro et al., 2003). It may explain the large variation of the CO abundance observed in comets and predicts an Ar/O ratio much less than the upper limit of 0.1 times the solar ratio estimated on C/2001 A2 (Weaver et al., 2002). Under the assumption that the amount of water ice present at 5 AU was higher than the value corresponding to the solar O/H ratio by a factor 2.2 at least, the clathration scenario reproduces the quasi uniform enrichment with respect to solar of the Ar, Kr, Xe, C, N and S elements measured in Jupiter by the Galileo probe. The interpretation of the non-uniform enrichment in C, N and S in Saturn requires that ice was less abundant at 10 AU than at 5 AU so that CO and N₂ were not clathrated in the feeding zone of the planet while CH₄, NH₃ and H₂S were. As a result, the 14N/15N ratio in Saturn should be intermediate between that in Jupiter and the terrestrial ratio. Ar and Kr should be solar while Xe should be enriched by a factor 17. The enrichments in C, N and S in Uranus and Neptune suggest that available ice was able to form clathrates of CH₄, CO and the NH₃ hydrate, but not the clathrate of N₂. The enrichment of oxygen by a factor 440 in Neptune inferred by Lodders and Fegley (1994) from the detection of CO in the troposphere of the planet is higher by at least a factor 2.5 than the lower limit of O/H required for the clathration of CO and CH4 and for the hydration of NH₃. If CO detected by Encrenaz et al. (2004) in Uranus originates from the interior of the planet, the O/H ratio in the envelope must be around of order of 260 times the solar ratio, then also consistent with the trapping of detected volatiles by clathration. It is predicted that Ar and Kr are solar in the two planets while Xe would be enriched by a factor 30 to 70. Observational tests of the validity of the clathration scenario are proposed.     

原位钛基复合材料中TiB的生成热力学及动力学

采用自蔓延高温合成（SHS）、感应熔炼和熔模精铸相结合的方法，利用Ti—B—Al体系制备出了原位自生TiB增强的钛基复合材料。借助XRD、SEM和TEM分析了复合材料的物相和增强体的形态。结果表明：在复合材料中只存在TiB增强体和Ti，无TiAl3杂质相形成，TiB增强体呈柱状短纤维，这与其B27晶体结构有关，且增强体／基体界面清洁无杂质污染，并从热力学和动力学两方面论述了在Ti—B—Al体系中制备TiB增强体的生成机制：在Ti-B—Al体系中，Al首先受热熔化使得Ti和B相继溶解于Al液中；Ti与Al之间先行发生化学反应形成Ti—Al金属间化合物，放出的热量进一步引发了溶解于液相中的B和Ti产生高温自蔓延形成Ti—B化合物。以热力学理论分析，应最终形成TiB2，但实际上由于动力学影响，最终形成了TiB。     

L10-TiAl金属间化合物Mn,Nb合金化电子结构的计算

采用第一原理赝势平面波方法计算了L10型TiAl金属间化合物中掺入Mn,Nb后的电子结构和价键结构.通过合金原子形成热得出Mn优先占据Al点阵位置,Nb优先占据Ti点阵位置.Mulliken聚居数分析发现Mn或Nb合金化后,分别降低了(001)和(002)面内的原子间键合强度,掺入Nb还降低了层间的原子间键合强度,而掺入Mn,则使层间原子间键合强度增加.整体上来讲,掺入Mn有利于改善TiAl的室温脆性,而掺入Nb,不利于改善TiAl的室温脆性.     

热压罐成型复合材料复杂结构对制造缺陷的影响规律

 飞行器复合材料种类多、结构形式复杂,制造缺陷种类、形成机制及影响因素也较为复杂。基于大量复合材料制件无损检测数据的统计结果,分析了热压罐成型工艺中常见缺陷的类型,揭示了复合材料复杂结构对制造缺陷的影响规律,初步分析了缺陷的产生机制。结果表明,分层、气孔和孔隙是热压罐成型工艺中比例较高的3类缺陷,复合材料制件结构的复杂性直接影响缺陷的出现比例,复合材料制件的几何特征和成型工艺对制造缺陷的影响规律较为明显。研究结果对制造缺陷的控制及复合材料制件结构设计具有重要的指导意义。     

考虑执行机构误差的编队卫星姿态分布式时延滑模自适应协同控制

针对编队卫星姿态协同控制问题,在考虑到执行机构误差的前提下,提出一种将时延控制与滑模自适应控制相结合的鲁棒控制方法.该方法通过引入自适应更新律实现对执行机构小角度安装误差的在线估计,同时通过滑模控制完成对外界干扰和执行机构随机幅值误差等随机扰动的抑制.由于引入了时延环节,只需对上一时刻控制力矩进行单位时延,达到大大简化...     

基于模糊专家系统的编队防空辅助决策系统

应用模糊推理理论的思想和方法设计和实现了编队防空辅助决策专家系统.文章详细介绍了系统的基本结构、知识表示和推理机制.系统采用模糊关系矩阵和基于框架的模糊推理相结合的推理方法,具有较高的准确性.最后给出了一个应用实例.     

编队卫星队形重构防碰撞最优轨迹规划

 针对编队卫星队形重构的轨迹规划问题,提出了直接配置混合整数线性规划(DCMILP)方法。首先将卫星编队飞行问题进行简化,整个过程使用线性化描述;继而将三阶Simpson方法扩展至编队卫星的队形重构过程中,将各卫星的状态量和控制量在各节点处离散化;然后根据目标函数及碰撞规避问题等各种约束条件,将整个过程转化为混合整数线性规划问题,从而可以找到该非凸问题的全局最优解。最后,通过对三维和二维两组编队卫星队形重构进行仿真,由结果可以看出,与传统方法相比该方法快速有效,能够满足实时性的要求,使得卫星编队的自主运行成为可能。     

纳米石墨薄片的制备、表征与应用

为了获得适宜于同聚合物进行纳米复合的纳米石墨薄片(NGS),采用微波膨化制备膨胀石墨(EG),利用超声剥离与表面修饰获得NGS,并借助SEM、XRD、FTIR等分析其微观结构。结果表明:EG由许多厚100-300 nm的石墨薄片连接而成并形成网络结构,孔隙尺寸约几十纳米到几十微米;通过对EG的超声剥离可破坏其原有网络结构并将石墨晶片进一步剥离为大量30-60 nm厚的石墨薄片;石墨微波膨化与超声剥离过程中微观形貌的变化及其表面活性基团的引入,有利于进一步借助插层法实现聚合物与石墨的纳米复合。     

基于相对轨道要素的航天器相对运动碰撞分析

采用基于相对轨道要素的方法,建立了计算碰撺概率的数学模型.在二体圆轨道条件下,推导验证了与基于Clohessy-wiltshire(C-W)方程的碰撞模型的等价关系,并解决了C-W方程存在的若干问题.在航天器近距离相对运动构型设计中提出了基于相对轨道要素的碰撞分析方法,突出了相对轨道要素在构型设计以及碰撞分析中的作用....     

国外空中加油技术的发展和展望

在简要地回顾了空中加油技术产生的背景和发展过程之后，较详细地介绍了其在空战中的实际应用和海湾战争时期各参战国的加油机装备情况，然后着重叙述目前世界上使用的两种空中加油系统（伸缩套管式加油设备和插头锥管式加油设备）；空中加油飞行技术和曾经进行的主要试验项目，未来空中加油机的发展趋势及尚待解决的问题。