未知互耦条件下混合信号波达方向估计

阵列天线互耦对导向矢量的扰动以及信号相干性对数据协方差矩阵造成的秩损,使得基于子空间正交性原理的超分辨波达方向估计(Direction-of-Arrival,DOA)算法性能恶化,甚至失效。针对这一问题,提出一种在相干与非相干信号混合状态下无需阵列互耦补偿的特征矢量平滑DOA估计算法。该算法对部分阵元接收数据的协方差矩阵特征分解,将得到的特征矢量平滑处理后构造等效协方差矩阵,抑制阵列互耦影响的同时完成混合信号DOA估计。在阵列互耦和信号相干性均未知的条件下,正确估计了信号DOA,无需互耦参数估计或补偿。计算机仿真结果验证了算法的有效性。     

直扩测控系统抗多址能力分析与验证

为了防止多址干扰造成接收机出现误捕和假锁,改善直接序列扩频测控系统抗多址干扰性能,在Gold码特性和扩频接收机性能分析的基础上,结合最大似然原理,对采用扩频体制测控系统的抗干扰能力进行了分析。为契合工程应用,采用仿真遍历结合理论分析的方式,对Gold码的互相关抑制能力理论值进行了工程修正。在分析捕获阶段的抗干扰捕获门限后,还分析了载噪比估计结果在正常锁定和假锁两种状态下的差异,给出了接收机对假锁状态的判决方法和门限。根据分析和仿真的结果,给出了系统设计约束条件和优化的接收机设计流程,作为测控系统和接收机设计的参考。     

粗糙表面偏振二向反射分布函数的影响参数及其反演

针对目标偏振二向反射特性研究中模型参数难以准确确定的问题,分析了粗糙表面偏振二向反射分布函数的影响参数,并通过理论推导和仿真计算,研究了各参数对粗糙表面散射特性的作用机理。总结分析了现有参数反演方法,针对现有方法存在的理论缺陷,在P-G(Preist-Germer)模型的基础上,提出了利用"相对偏振分量-角度"的相关关系进行参数反演的方法,设计了参数反演算法,进行了标准反射板和绿漆表面的偏振二向反射特性测试实验,并根据实验数据进行了参数反演和模型验证。实验结果表明,改进的参数反演方法可准确反演所有模型参数。利用反演参数进行模型验证,结果显示模型预测数据与实验数据具有较好的吻合度,验证了模型的准确性。     

用户星中继终端在轨应用策略

在介绍在轨用户星中继终端的分类、功能和使用现状的基础上,重点对用户星中继终端多约束条件进行了梳理分析。为缓解常态化应急测控带来的资源紧张矛盾,提出了用户星中继终端在轨应用策略,即Ka/S模式下影随测控,小S模式下定时捕获。针对Ka+小S模式下实现影随测控的可行性问题,利用STK(Satellite Tool Kit,卫星开发工具包)软件进行了仿真计算分析,结果表明:为实现影随测控,满足测控快速响应需要,要求星载S频段中继测控天线对中继卫星的覆盖范围,应大于星载中继数传天线对中继卫星的覆盖范围。     

波音777飞机ACARS系统及马航MH370航班失联事件分析

马来西亚航空公司MH370客机失联事件一度引发媒体与公众的诸多猜测,猜测的焦点之一就是执飞的波音777飞机的飞机通信寻址与报告系统(Aircraft Communication Addressing and Reporting System,简称ACARS)功能是如何被关闭的。从专业角度出发,首先采用Sys ML建模的方式描述了波音777飞机ACARS系统的详细架构和人机接口,并据此深入分析了马航MH370航班失联事件中ACARS被关闭的情景。最后,提出了此次事件暴露出的现代民用飞机设计中存在的问题以及改进方法。     

论航空公司客户关系管理的发展方向

介绍了客户关系管理（cRM）理论，研究了国内外航空公司发展CRM的历史，并重点分析了国内航空公司在客户关系管理上存在的主要问题和解决方案，最后根据CRM理论阐述了航空公司客户关系管理的发展方向。     

某型导弹控制舱壳体机械加工技术研究

结合生产实践介绍了新一代导弹的重要构件－控制舱壳体机械加工的难点及其工艺总方案的确定，并着重就控制铝合金乐于壁壳体的变形、提高偏心圆加工精度的措施进行了细致的研究，实践证明，该种工艺方法简单、合理，可以为类似的复杂舱体加工提供一条可借鉴的工艺途径。     

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.     

Near infrared studies of the massive X-ray binary 2S 0114+65

We present near-infrared spectroscopy of the massive X-ray binary 2S 0114+650. These observations covering the spectral range 1.08–2.35 μm span the region where Paschen and Brackett series recombination lines of hydrogen are expected to be seen, namely, Paβ , Brγ and Br 10–17 lines. The absence of any of these lines in emission supports earlier inferences that the optical component in 2S 0114+650 is unlikely to be a Be star but rather a B type supergiant. Near-IR photometry gives J = 8.78, H = 8.53 and K = 7.96; these values show marginal variations from earlier reported measurements.     

Keck observations of ROSAT ultra-luminous X-ray source candidates

We present results of optical follow-up observations of candidate ultra-luminous X-ray sources (ULXs). Using Keck optical spectroscopy, 17 of the candidates from the Colbert and Ptak [Colbert, E.J.M., Ptak, A.F. A catalog of candidate intermediate-luminosity X-ray objects. ApJS 143, 25–45, 2002] catalog have been identified; this is one of the largest sets of optical identifications of such objects thus far. Fifteen are background active galactic nuclei (AGN); two are foreground stars in our Galaxy. These findings are consistent with background and foreground object expectations, as derived from log N–log S relations. Also, the results are briefly discussed in terms of the spiral-galaxy/ULX connection.