The Origin of Mercury

Mercury’s unusually high mean density has always been attributed to special circumstances that occurred during the formation of the planet or shortly thereafter, and due to the planet’s close proximity to the Sun. The nature of these special circumstances is still being debated and several scenarios, all proposed more than 20 years ago, have been suggested. In all scenarios, the high mean density is the result of severe fractionation occurring between silicates and iron. It is the origin of this fractionation that is at the centre of the debate: is it due to differences in condensation temperature and/or in material characteristics (e.g. density, strength)? Is it because of mantle evaporation due to the close proximity to the Sun? Or is it due to the blasting off of the mantle during a giant impact? In this paper we investigate, in some detail, the fractionation induced by a giant impact on a proto-Mercury having roughly chondritic elemental abundances. We have extended the previous work on this hypothesis in two significant directions. First, we have considerably increased the resolution of the simulation of the collision itself. Second, we have addressed the fate of the ejecta following the impact by computing the expected reaccretion timescale and comparing it to the removal timescale from gravitational interactions with other planets (essentially Venus) and the Poynting–Robertson effect. To compute the latter, we have determined the expected size distribution of the condensates formed during the cooling of the expanding vapor cloud generated by the impact. We find that, even though some ejected material will be reaccreted, the removal of the mantle of proto-Mercury following a giant impact can indeed lead to the required long-term fractionation between silicates and iron and therefore account for the anomalously high mean density of the planet. Detailed coupled dynamical–chemical modeling of this formation mechanism should be carried out in such a way as to allow explicit testing of the giant impact hypothesis by forthcoming space missions (e.g. MESSENGER and BepiColombo).     

Modelling of Ejecta as a Space Debris Source

When a micro-debris or a micrometeoroid impacts a spacecraft surface, a large number of secondary particles, called ejecta, are produced. These particles can contribute to a modification of the debris environment: either locally by the occurrence of secondary impacts on the components of complex and large space structures, or at great distance by the formation of a population of small orbital debris. This paper describes firstly, the ejecta overall production, and secondly, the lifetime and the orbital evolution of the particles. Finally the repartition of ejecta in LEO is computed. Some results describing the population as a function of size and altitude are presented.     

空战机动动作库设计方式研究

具体阐述了两类常见空战动作库的设计 :典型战术动作库和基本操作动作库 ,详细分析了这两类空战机动动作库的不足 ,最后提出了改进动作库设计的具体意见和建议。     

滚珠丝杠螺距误差补偿法提高数控机床定位精度的研究

在详细论述、对比了实现数控机床滚珠丝杠螺距误差补偿的硬件、软件方法的原理基础上,对滚珠丝杠螺距误差软件补偿法可有效提高数控机床的定位精度进行了试验验证。     

低空突防任务下综合飞行/推进系统的建模与仿真

建立了综合飞行／推进系统的数学模型，介绍了飞机全维非线性数学模型和涡轮风扇发动机非线性部件级数学模型的建模及综合方法。对飞机执行地形中随任务时，飞行员调节飞行速度的方法与基于总能量的调节飞行速度的方法进行了比较。结果表明，基于总能量的方法比飞行员直接控制飞行速度能够减小发动机的燃油消耗，降低发动机的磨损，进而可以增加飞机的航程，延长发动机的使用寿命。     

四维下降飞行技术的研究与仿真：定常航迹角法下降剖面解算

本文研究的是四维飞行性能管理系统的核心环节－飞机在终端区域内的四维下降技术，首先探讨了基于常值航迹角的定常Ｍ数／指示空速下降飞行技术，论述了其高度剖面的构成与特点，通过尤拉积分方法求解飞机运动方程，实现了高度冲面的解算。其次开发了对速度剖面的迭代过程，选取原则及方法。本文在进行理论分析的同时，还开发了满意的仿真软件，一了其应用价值。     

航电系统SCI环型互连的计算机仿真建模

研究可扩展一致性接口 SCI环型互连的计算机仿真问题。作为未来一代航电系统的首选技术 ,SCI互连系统性能的优劣直接影响到飞行器的质量 ,对其性能的评价因此显得尤为重要。文中按照计算机仿真建模的一般方法 ,从 SCI协议的基本原理出发 ,建立了接口和节点模型 ,解决了并发数据交互的仿真时序问题 ,给出了 SCI环型互连的系统仿真模型 ,并通过例子对仿真模型的有效性进行了验证     

锥柱形加筋金属膜片变形的数值仿真分析

概述了金属膜片贮箱膜片结构的研究现状,提出了锥柱形加筋膜片整体结构变形问题。根据试验情况建立了该膜片的有限元模型,并基于非线性有限元软件MSC.Marc进行了数值模拟,分析了膜片结构的变形过程和变化规律,通过对加筋结构的分析解释了膜片变形的机理,得到了一些控制膜片失效的方法。     

发动机数控系统含实物电子仿真

发动机数控系统含实物电子仿真是用真实的数字控制器与发动机实时数学模型构成闭环仿真系统，控制器接口所需要的各种传感器信号及机械液压供油装置和喷口控制装置由电子模模拟，从而为数字控制器提供基本运行环境。本文研究了发动机数控系控制规律和控制逻辑，，检测了数字控制器软件硬件的工作性能，表明含实物电子仿真试验具有试验成本低，风险小等特点，是发动机数字控制器研制过程中一个重要环节。     

高速列车绕流的数值模拟

给出了用低速N－S方程求解高速列车绕流的数值计算方法，采用显隐式结合的方法来加快收敛速度，基于该方法编制了计算软件系统Train3D，用该软件系统对高速列车外形的外流场进行了数值模拟，获得了该外形的空气动力特性和流场结构。