红外窗口内冷防热机理及其性能预测

给出了红外窗口内冷防热机理和防热性能预测.以液氨作为冷却剂在窗口内通道流动,利用液氨由液态转化为气态的相变过程中大量吸热的特性,达到冷却窗口的目的.并采用有限元方法计算外部具有对流加热,内部有冷却剂吸热的窗口材料温度分布.本文计算结果与地面电弧加热器实验测量结果作了比较,两者较为吻合,验证了防热预测方法的可行性.     

压力恢复系统扩压器激波串现象的数值模拟

通过求解由S-A一方程湍流模式封闭的三维雷诺平均Navier-Stokes方程,采用有限体积方法对激光器压力恢复系统变截面扩压器常温状态下的三维流场进行了数值模拟.数值计算和实验符合良好,较好模拟了扩压器中由激波/边界层干扰诱导的复杂流场的流场特性并再现了流场中的"激波串"和"伪激波"现象.本文对激波串的形成机理进行了分析,发现了几种变截面扩压器特有的激波串结构,并研究了扩压器扩张角对扩压效率的影响.     

Cu-1.0% Cr亚共晶合金定向凝固组织演化

在定向凝固下计算和比较了Cu-1.0%Cr亚共晶合金组织中各相的界面生长温度,结果表明当定向凝同速率大于5αm/s时,α-Cu相的界面生长温度高于共晶组织,α-Cu相会作为初生相首先析出凝固,从而难以制备出全耦合生长的共晶组织的复合材料,计算获得的结果与实验结果相一致.另外随定向凝固速率的增加,初牛胞状α-Cu相一次枝晶间距和尖端半径以及共晶组织的体积分数都相应地减少,其中α-Cu相一次枝晶间距实验结果与KF一次枝晶间距模型计算结果较为接近.     

燃气发生器结构对燃烧性能的影响

为了确定最佳的燃气发生器结构,对不同结构的燃气发生器进行了对比试验,考察了喷嘴尺寸、燃烧室长度、燃烧室构型等因素对燃气发生器燃烧性能的影响.研究结果表明:在一定范围内增大喷嘴尺寸,燃烧性能基本不受影响,但却可以缩短燃气发生器的点火延迟时间,并且增大流量调节范围;增加燃烧室长度可以明显的提高燃烧效率;燃烧室的构型对燃烧性能有很大影响,收缩-扩张型着火段影响了燃烧过程,降低了燃烧效率,燃气发生器设计不宜采用这种构型.      

故障星分布对星座PDOP可用性影响的建模及评价

 导航星座定位精度衰减因子（PDOP）可用性是卫星导航系统顶层设计的重要指标。研究了不同故障星分布状况对全球导航星座PDOP可用性的影响。首先,从概率角度并采用组合方法建立了全球导航星座PDOP可用性指标的统计评价模型。进而对给定数量的故障星分布在单个或多个轨道面内的不同状况下,典型的Walker δ构型导航星座的PDOP可用性如何变化进行了仿真计算和比较分析。仿真结果表明,故障星分布状况和轨道平面数对星座PDOP可用性有较显著影响,适当地减少轨道平面数对于改善星座的PDOP可用性是有利的。提出的评价模型物理意义明确,避免了主观性和局限性,且可以保证较高的指标评价效率。     

RS码的时域编码频域译码技术

通过对于RS码的时域编码／频域译码的算法进行分析,找到了它们的不同之处及转换方法,得出了时域编码／频域译码的混合编译码方法,提高了运算速度和纠错能力。     

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.     

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.