星用材料出气加速规律扩散模型

基于扩散理论分析获得了星用材料在一定温度范围内出气加速过程遵循的规律，给出了加速系数与扩散系数，加速系数与出气过程等当时间及与温度之间的函数关系，并经实验测试证明，理论分析结果克能良好反映材料出气加速过程所遵循的规律。     

飞行加速度对固体发动机后封头绝热层烧蚀的影响

固体火箭发动机后封头绝热层的炭化烧蚀率与飞行加速度有关。概述了国内外在这方面的一些研究情况，着重讲述了固体火箭发动机后封头内绝热层烧蚀的实验研究。实验表明：不同材料的绝热层在加速度作用下烧蚀率明显不同。在加速度作用下，后封头内绝热层的炭化烧蚀率小于静止状态的炭化烧蚀率。     

直升机动力学中参数振动问题的数值解法

 参数振动问题是直升机的基本动力学问题之一,旋翼桨叶的挥舞弯曲微分方程和摆振弯曲微分方程都是复杂的参数振动问题,在许多计论直升机旋翼动力学的论著中~[1-4],有的虽然推导了复尽杂的参数振动方程,却没有提到求解的方法,有的对此根本没有论及.本文旨在讨论参数问题的数值解法.     

高过载条件下绝热层烧蚀实验方法研究 (Ⅰ)方案论证及数值模拟

分析了高过载对固体火箭发动机流场和绝热层烧蚀的影响规律，提出一种新的研究思路：采用数值模拟方法来预示发动机三维两相流场，建立高过载流场模拟实验装置，开展绝热层烧蚀实验，建立高过载条件下的绝热层烧蚀模型，在此基础上发展高过载发动机绝热层设计和烧蚀预示方法。其中关键技术是高过载流场的模拟，对粒子加入法和弯管分离法两种方案进行了论证，认为弯管分离法原理上是可行的。为了验证这种方案的可行性，开展了弯管通道两相流的数值模拟研究，计算结果表明弯管装置具有使凝相粒子聚集形成高浓度粒子流的功能。     

基于人工免疫的直升机传动系统在线异常监测方法

 针对直升机在线监测时难以提取状态特征的问题，提出一种适用于直升机传动系统在线状态监测方法。该方法基于生物免疫系统反面选择机理，利用改进型反面选择算法并结合人工神经网络进行监测。该方法能有效地提取直升机传动系统的状态特征，并结合直升机传动系统的实际情况准确得出状态异常度。在线监测实例结果表明，该方法能较准确监测出直升机传动系统的异常状态，验证了该方法具有较好的在线性、准确性及鲁棒性。     

某型飞机后减速板振动试验

某型飞机后减速板在部队使用中多次出现减速板梁断裂、蒙皮裂纹等故障 ,打孔加型材结构改进方案经实际飞行测试取得了满意效果。为给出打孔加型材结构改进方案的使用寿命 ,进行了 2种结构后减速板的地面振动对比试验。本文对后减速板地面振动对比试验方法进行简要介绍。     

Flight Flutter Modal Parameters Identification with Atmospheric Turbulence Excitation Based on Wavelet Transformation

针对基于大气紊流激励的飞机颤振试验数据具有信噪比低以及测量数据以加速度响应形式给出等特点,将小波变换与随机减量法相结合对飞机颤振模态参数进行识别,首先利用随机减量法获得结构在非零初始加速度条件下的自由衰减响应,然后对该自由衰减响应进行Morlet连续小波变换,为使变换简单,本文采用了Parseval定理和留数定理,利用Morlet的带通滤波特性,通过搜索小波变换系数在不同的尺度区域内的极大值,再根据小波变换系数的极大值、相角与固有振动频率及阻尼系数间的关系,即可识别出各模态参数。并对利用小波变换识别颤振模态参数时,实现模态解耦应满足的条件进行了分析研究。通过仿真和飞机颤振试验数据分析,验证了该识别方法不仅简单、有效和可行,而且具有较强的抗噪性。     

关于刚体转动的角速度和角加速度的讨论

在理论力学教学中，平面运动刚体的转动与基点无关的证明过于简单，本利用矢量代数的知识，证明平面运动刚体的角度与角加速度与基点的选择无关。     

涡喷发动机加速控制系统数学模型及数字仿真

 本文介绍了航空涡轮喷气发动机加速控制系统数学模型建立、数字仿真方法。由于加速过程是一个大偏离动态过程,因而发动机与加速控制器模型均用非线性方程描述,对非线性方程组求解和系统迭代方法本文进行了讨论。算例中分析了在不同飞行条件下发动机的加速规律。     

MESSENGER: Exploring Mercury’s Magnetosphere

The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission to Mercury offers our first opportunity to explore this planet’s miniature magnetosphere since the brief flybys of Mariner 10. Mercury’s magnetosphere is unique in many respects. The magnetosphere of Mercury is among the smallest in the solar system; its magnetic field typically stands off the solar wind only ∼1000 to 2000 km above the surface. For this reason there are no closed drift paths for energetic particles and, hence, no radiation belts. Magnetic reconnection at the dayside magnetopause may erode the subsolar magnetosphere, allowing solar wind ions to impact directly the regolith. Inductive currents in Mercury’s interior may act to modify the solar wind interaction by resisting changes due to solar wind pressure variations. Indeed, observations of these induction effects may be an important source of information on the state of Mercury’s interior. In addition, Mercury’s magnetosphere is the only one with its defining magnetic flux tubes rooted beneath the solid surface as opposed to an atmosphere with a conductive ionospheric layer. This lack of an ionosphere is probably the underlying reason for the brevity of the very intense, but short-lived, ∼1–2 min, substorm-like energetic particle events observed by Mariner 10 during its first traversal of Mercury’s magnetic tail. Because of Mercury’s proximity to the sun, 0.3–0.5 AU, this magnetosphere experiences the most extreme driving forces in the solar system. All of these factors are expected to produce complicated interactions involving the exchange and recycling of neutrals and ions among the solar wind, magnetosphere, and regolith. The electrodynamics of Mercury’s magnetosphere are expected to be equally complex, with strong forcing by the solar wind, magnetic reconnection, and pick-up of planetary ions all playing roles in the generation of field-aligned electric currents. However, these field-aligned currents do not close in an ionosphere, but in some other manner. In addition to the insights into magnetospheric physics offered by study of the solar wind–Mercury system, quantitative specification of the “external” magnetic field generated by magnetospheric currents is necessary for accurate determination of the strength and multi-polar decomposition of Mercury’s intrinsic magnetic field. MESSENGER’s highly capable instrumentation and broad orbital coverage will greatly advance our understanding of both the origin of Mercury’s magnetic field and the acceleration of charged particles in small magnetospheres. In this article, we review what is known about Mercury’s magnetosphere and describe the MESSENGER science team’s strategy for obtaining answers to the outstanding science questions surrounding the interaction of the solar wind with Mercury and its small, but dynamic, magnetosphere.