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.     

基于SFEM的SRM纤维缠绕结构的可靠性分析

采用纽曼级数展开的蒙特卡罗随机有限元方法(SFEM),分析了固体火箭发动机(SRM)复合材料缠绕的燃烧室在内压正态变化下的应力响应,然后利用应力强度干涉原理分析计算其可靠性.     

一种涡轮发动机加速控制规律设计的新方法

 提出了一种涡喷、涡扇发动机加速控制规律快速设计的新方法：在发动机稳态特性计算模型的基础上,通过额外增加转子提取功率,使得发动机稳态工作点（线）靠近喘振边界,在同时考虑燃烧室富油熄火边界、涡轮进口总温限制以及压气机喘振裕度限制的条件下,利用适当的控制规律描述形式并结合发动机工程研制中的经验,能够快速而准确地获得涡喷、涡扇发动机加速控制规律。对某型涡喷发动机加速控制规律的改进的计算结果表明,提出的加速控制规律的设计方法准确而有效。     

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.     

在单脉冲内利用Hough-Ambiguity变换估计目标加速度研究

根据雷达发射恒定载频信号时匀加速目标的回波为线性调频（LFM）信号的特点,研究了在单脉冲内基于Hough—Ambiguity变换（HAT）估计目标径向加速度的问题。首先,采用Hough—Ambiguity变换得到信号的调频斜率;进而,根据调频斜率估计出目标径向加速度;最后,仿真实验结果验证了方法的有效性。     

退化发动机加速性能恢复控制方法

针对退化发动机加速性能下降的现象,提出一种变喘振裕度约束的模型预测控制方法。通过分析退化发动机在加速过程中的工作特点,将加速过程分为三个阶段,在不同阶段采取不同的喘振裕度约束。鉴于模型预测控制能够显式处理约束、采用在线滚动优化来获取最优控制输入,采取模型预测控制方法,并采用具有较高实时性的交替方向乘子法求解优化问题,实现了退化发动机加速性能的恢复。数字仿真结果表明,采用本文所提出的加速性能恢复控制方法后,相比退化发动机,加速过程中所耗费的时间缩短了35%以上。     

基于载荷当量安装误差的面齿轮振动特性

以面齿轮传动系统为研究对象,考虑载荷作用下面齿轮传动系统中支撑结构变形和轮齿弹性变形,通过将传动系统变形等效到面齿轮和直齿轮安装误差方向,建立包含当量安装误差的面齿轮多自由度耦合振动分析模型;采用4阶Runge-Kutta法求解了面齿轮传动系统运动微分方程,得到了当量安装误差对面齿轮振动加速度和法向动态啮合力的影响;开展了面齿轮动态特性测试试验,试验结果表明:偏置距误差和轴交角误差引起的面齿轮沿x方向振动加速度大于沿z方向振动加速度;偏置距误差对面齿轮x方向振动加速度的影响大于轴交角误差。      

磁激等离子体超声速气流的瞬态加速系统及其实验研究

研制了基于激波风洞的热电离系统,设计了马赫数Ma=1.5的喷管和分段法拉第型实验段,并选用了合理的磁场及电场方案。采用氦气驱动氩气模式,通过在激波管低压段注入电离种子K₂CO₃粉末实现气流的热电离;压缩后的高温氩气启动喷管,以瞬态超声速导电流体形式通过实验段。实验结果表明:当激波管高压段压力为1.1 MPa、低压段压力为500 Pa时,喷管出口的超声速导电气流温度约为4 185.91 K,压力约为0.037 MPa;当电容电压为400 V、磁感应强度为1.0 T时,由实验段中间位置电极的放电特性可以估算出气流电导率约为78.1 S/m,单对电极输入功率约为9.46 kW;用感应电压法对加速效果进行初步评估,出口气流速度增加了29.3%,电效率为26.1%。