火星大气进入段抗饱和固定时间阻力加速度跟踪制导律设计

研究了具有固定时间收敛特性的火星探测器大气进入段的标称轨迹跟踪制导问题。首先,针对横向运动,给出与速度成线性关系的航向误差漏斗走廊形式,完成了倾侧角的反号逻辑设计。与横程漏斗走廊反号逻辑相比,该逻辑计算量小,更适用于宇航计算机。与航向误差宽度走廊反号逻辑相比,该逻辑在高速状态下能够避免倾侧角的频繁切换,可提高任务成功的概率。其次,针对纵向运动,通过RBF神经网络补偿了倾侧角饱和问题,利用积分滑模设计了阻力加速度固定时间饱和跟踪制导律,其不仅可有效消除滑模控制的抖振问题,且将跟踪误差以两种不同形式引入制导律,能够加速收敛,能够保证跟踪误差在固定时间内快速收敛至0。最后,通过数值仿真验证了所设计的横向倾侧角切换逻辑和纵向制导律对标称轨迹的快速、精确跟踪能力。     

基于加速度测量的智能桁架结构振动主动控制

加速度传感器具有频带宽、结构简单、重量轻等优点而获得了广泛使用,因此研究基于加速度测量的结构控制系统具有较大的实用价值。文中的只能获得加速度时,采用模态滤波器技术实现从物理加速度响应解耦得到单模态加速度的响应。然后改变Ｌｕｅｎｂｅｒｇｅｒ观测器的结构形式,从模态加速度响应观测得到模态们移和模态速度响应。基于模态滤波器和最优控制理论,采用独立模态空间控制策略,实现了具有密集模态的三维柔性智能桁架结构     

微制造隔振试验平台定位系统的轨迹规划

为减小运动部件加减速过程中对整个平台的冲击,在进行运动轨迹规划时,采用了S形曲线对定位系统的运动轨迹进行了平滑处理,有效地降低了运动部件对系统的冲击,有利于系统的减振。     

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。     

多重应力下滚动轴承剩余寿命预测

为了实现多重应力下滚动轴承的剩余寿命预测,有效利用不用应力下的退化数据,提出了一种基于加速模型和贝叶斯（Bayesian）理论的滚动轴承剩余寿命预测方法。通过拟合优度检验和威布尔（Weibull）概率图检验法对滚动轴承试验中的数据进行有效性分析。利用switching Kalman filters(SKF)判断滚动轴承各时刻的退化状态。当滚动轴承进入加速退化时,用指数模型拟合轴承退化过程,利用广义线性对数模型表示退化模型参数与应力的关系,根据修正后的轴承实时退化数据利用贝叶斯算法更新模型参数,得到滚动轴承剩余寿命的概率密度函数,从而实现滚动轴承剩余寿命预测。采用XJTU-SY轴承数据集进行验证,预测结果的均方根误差在20 min以内,证明该方法能够有效预测滚动轴承的剩余寿命。     

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。     

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。     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

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.     

Galactic Wind: Mass Fractionation and Cosmic Ray Acceleration

The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×10¹⁸ eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall Cosmic Ray spectrum.