旋翼气动提前操纵角研究

为了保证某型直升机操纵系统设计的顺利进行,本文基于国内外相关资料对气动提前操纵角进行了深入的研究,得出该角度主要取决于桨叶挥舞基阶固有频率ωβ1.而ωβ1与挥舞铰外伸量e、桨叶根部弹性约束Kβ和挥舞调节系数Kp密切相关.通过分析e,Kβ和Kp对气动提前操纵角△ψ的影响,推导出计算该角度的具体公式.采用该公式对几个型号进行计算,经校核与验证后,表明本文提供的计算方法可行,能满足工程精度,可应用于工程研究,从而为布置助力器提供理论依据.     

RLV再入姿态双环滑模控制及舵喷混合配置

应用滑模控制设计了一种可重复使用运载器（RLV）再入姿态控制器,该控制器应用双环的滑模控制方案,可以获得对角速度及角度的同时跟踪,并具有较好的鲁棒性和解耦性能。针对RLV再入姿态的动力面与反作用混合控制的特点,运用优化控制选择配置算法把控制力矩指令配置为末端受动器的控制指令,分别由动力面与反作用致动器来执行。再入姿态仿真验证了该方法的精度、鲁棒性以及解耦的跟踪性能及有效性。     

高超声速战术导弹精确制导律设计

高超声速战术导弹以其固有的特点在高速目标拦截上应用前景巨大.如何针对高超声速战术导弹高速度、高不确定性的特点设计精确的制导律是导弹能否摧毁目标的关键.针对高超声速战术导弹和高速机动目标建立了相对运动模型,利用自适应滑模控制理论,设计了导弹的自适应精确制导律,并进行了仿真分析.结果表明,该制导律具有较好的控制效果.     

飞行器控制分配技术研究现状与展望

综述了现代飞行器控制分配技术的研究和应用状况.首先简要回顾了线性控制分配方法,然后着重论述了非线性控制分配技术的最新研究成果,包括截距修正法、分段线性规划法、非线性规划法及包含神经网络计算、遗传算法和模糊逻辑在内的智能控制分配技术,最后讨论了有待于进一步完善和深入研究的若干问题.     

灰度相关图像匹配算法噪声适应性仿真

文章主要研究基于灰度的图像匹配算法对于图像噪声的适应能力。首先对两种典型的基于灰度的图像匹配算法——ABS（Absolute Balance Search）法和归一化互相关法进行了简要介绍,随后通过仿真实验深入研究了上述两种算法对于图像噪声的适应能力;最后得出了相应的结论。     

高超声速飞行器后体喷管三维构型设计

为研究高超声速飞行器后体喷管三维构型的设计,以NASA半壁喷管试验为参考,进行了二维及三维内外流相互作用的数值模拟计算,分析了后体喷管三维流场的特点.从高超声速飞行器机身推进一体化的角度,构建了后体喷管三维构型,进行了不同构型设计对后体喷管性能影响的参数研究.结果表明:后体喷管的三维效应不可忽视,后体喷管侧壁的存在及下壁面长度对性能影响较大.      

某高超飞行器流道冷流特征及气动力特性研究

对一种类似于X-43A的吸气式高超声速一体化构形全流道开展了风洞实验和数值模拟研究,分析了不同来流总压、飞行攻角以来流Ma数下全流道的流场结构和气动力特性.研究结果表明:(1)飞行攻角对全流道的流动结构和升力系数有着显著影响,但阻力系数的影响并不明显;(2) 研究范围内来流马赫数的变化对全流道的流动结构和全机气动力特性有着一定影响;(3) 前体横截面上存在显著的展向压强梯度,使得经过预压缩的气流偏离了进气道进口,但同时也减少了进入内通道的边界层气流,提高了进口流场的品质.     

Fe/O Ratios in Interplanetary Shock Accelerated Particles

It is widely accepted that diffusive shock acceleration is an important process in the heliosphere, in particular in producing the energetic particles associated with interplanetary shocks driven by coronal mass ejections. In its simplest formulation shock acceleration is expected to accelerate ions with higher mass to charge ratios less efficiently than those with lower mass to charge. Thus it is anticipated that the Fe/O ratio in shock-accelerated ion populations will decrease with increasing energy above some energy. We examine the circumstances of five interplanetary shocks that have been reported to have associated populations in which Fe/O increases with increasing energy. In each event, the situation is complex, with particle contributions from other sources in addition to the shock. Furthermore, we show that the Fe/O ratio in shock-accelerated ions can decrease even when the shock is traveling through an Fe-rich ambient ion population. Thus, although shock acceleration of an Fe-rich suprathermal population has been proposed to explain large Fe-rich solar particle events, we find no support for this proposal in these observations.     

基于放气控制的飞机轮胎自动充气装置设计

根据国内飞机轮胎充气工作的现状,设计了一种基于放气控制的飞机轮胎自动充气装置,介绍了基于此种方式的充气及检测控制过程,针对以往充气装置的不足,此控制方式能够提高轮胎充气及检测的精度。并通过实验证明系统设计合理,满足设计要求,且系统效率高、性能稳定、操作方便,具有较好的经济效益及社会效益。     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.