飞机下滑波束导引系统设计及仿真

下滑波束导引系统是飞机在自动着陆时所采用的一种重要无线电波束导引系统。首先,简要阐述了下滑波束导引系统的基本工作原理;然后,对导引系统的运动学环节及下滑耦合器进行分析,对飞机下滑波束导引系统结构进行设计;最后,在MATLAB平台下,对所设计的下滑波束导引系统进行大量仿真研究。仿真结果显示。所设计的下滑波束导引系统结构是合理的,其控制系统是稳定的,且其稳态性能也得到改善。     

分开排气系统的1种设计方法及其性能研究

针对大涵道比涡扇发动机,开展了其排气系统气动型面参数化设计方法和气动性能的研究。通过控制外涵、内涵喷管流道的中心线形状和流通面积,设计了外涵、内涵分开排气喷管气动型面。采用数值模拟的方法模拟了喷管的流场结构,并分析了外涵落压比和自由流马赫数对喷管推力系数的影响。在自由流马赫数为0.050时,推力系数随外涵落压比的增大而增大,在自由流马赫数为0.785时,推力系数随外涵落压比的增大而减小;在外涵落压比相同时,自由流马赫数越大,核心机舱外罩b段与尾锥b段所受轴向力在喷管总推力中所占比例越大,对喷管推力系数的影响也增大。     

基于技术参数评估的涡扇发动机总体性能设计分析

为了充分掌握各代涡扇发动机技术参数水平及其发展趋势,统计包括现役型号在内的15台2～4代涡扇发动机的总体性能参数、循环参数和部件参数,采用考虑涡轮冷却的总体性能计算和重量预测相结合的发动机技术参数综合评估模型并利用计算程序绘制趋势曲线,评估技术参数的发展趋势,结果表明技术参数逐年改善的趋势是比较稳定的,并用曲线趋势外推法取得下一代关键参数的定量数据。在此基础上探索下一代高推重比涡扇发动机可能的总体性能方案,为下一代先进涡扇发动机的预研和设计提供参考。     

降低PLC系统峰均比的低复杂度改进SLM算法

针对信道慢时变特性及噪声复杂的特点,提出了适用于低压电力线通信的降低峰均比的改进算法.改进算法对原始输入序列中的部分数据进行循环移位来获得一系列不同的新数据序列;在每个新数据序列尾部插入相应的边带信息组成一个输入候选序列;对这一系列不同的输入候选序列分别实施傅里叶反变换,得到不同的输出序列;从中选择峰均比最小的用于传输,达到降低系统峰均比的目的.结果表明:改进算法能够有效地降低系统的峰均比,并且能够获得更好的误码率性能,同时具有比传统选择性映射方法更低的计算复杂度.     

卷帘行存储下的一种并行Cholesky分解及其在PAR95上的实现

Ｃｈｏｌｅｓｋｙ 分解在科学与工程计算中占有重要的地位，串行的 Ｃｈｏｌｅｓｋｙ 分解已有成熟的方法，但并行的 Ｃｈｏｌｅｓｋｙ 分解方法要充分考虑机器体系的结构，在拥有共享内存的 Ｍ Ｉ Ｍ Ｄ 型多处理机、 Ｓ Ｉ Ｍ Ｄ 型向量机系统上前人已有较好的工作，本文给出适用于 Ｍ Ｐ Ｐ 大规模并行计算机的卷帘行存储行格式的并行 Ｃｈｏｌｅｓｋｙ 分解算法，该算法使用了优先计算优先发送的策略，减少了结点机之间相互等待的时间，建立了结点机之间用于通讯的通讯数组，避免了使用撒播这一通讯模式，减少了通讯时间，通过在 Ｐ Ａ Ｒ９５ 上的数值试验表明，随着问题规模的扩大，并行效率越来越高，并且该法容易推广到多行卷帘存储的形式。     

Enhancing buckling capacity of a rectangular plate under uniaxial compression by utilizing an auxetic material

Auxetic materials have previously been shown to enhance various performances due to its unusual property of becoming fatter when uniaxially stretched and thinner when uniaxially com-pressed (i.e., the materials exhibit a negative Poisson’s ratio). The current study focuses on assessing the potential of an auxetic material to enhance the buckling capacity of a rectangular plate under uniaxial compression. The in-plane translational restraint along the unloaded edges that was often neglected in open literature is taken into consideration in our buckling model proposed in this study. The closed-form expressions for the critical buckling coefficient of the rectangle are provided and the predicted results agree well with those determined by the finite element method. Further-more, the results indicate that the buckling performance of a rectangular plate under uniaxial com-pression can be significantly improved by replacing the traditional material that has a positive Poisson’s ratio with an auxetic material when there is in-plane translation restraint along the unloaded edges.     

Evolution of the orbital elements for objects with high area-to-mass ratios in geostationary transfer orbits

A new population of uncatalogued objects in geosynchronous Earth orbits (GEO), with a mean motion of about 1 rev/day and eccentricities up to 0.6, has been identified recently. The first observations of this new type of objects were acquired in the framework of the European Space Agency’s (ESA) search for space debris in GEO and the geostationary transfer orbit (GTO) using the ESA 1-m telescope on Tenerife. Earlier studies have postulated that the perturbations due to the solar radiation pressure can lead to such large eccentricities for GEO objects with a high area-to-mass ratio (A/M). The simulations showed that the eccentricities of GEO objects with large A/M exhibit periodic variations with periods of about one year and amplitudes depending on the value of A/M. The findings of these studies could be confirmed by observations from the ESA 1-m telescope on Tenerife.     

波形记录仪触发延迟线性的实验研究

提出了使用正弦波激励评价触发延迟线性度和触发抖动的新方法，通过一个波形在有触发延迟和无触发延迟时，采集序列间的相位差对应的时间差来最终判定触发延迟结果。用该方法实现的触发延迟线性度测量方法，将触发延迟直接溯源到激励信号的频率量上，无需额外的精密延时器等装置，减少了测量环节，并且可以实现任意延迟的精确测量。以不同频率、不同触发延迟、不同采集速率下的实验结果的对比给出了触发延迟线性校准的结论性意见，同时验证了所述方法的有效性和切实可行性。     

Dynamical evolution of high area-to-mass ratio debris released into GPS orbits

A large set of simulations, including all the relevant perturbations, was carried out to investigate the long-term dynamical evolution of fictitious high area-to-mass ratio (A/M) objects released, with a negligible velocity variation, in each of the six orbital planes used by Global Positioning System (GPS) satellites. As with similar objects discovered in near synchronous trajectories, long lifetime orbits, with mean motions of about 2 revolutions per day, were found possible for debris characterized by extremely high area-to-mass ratios. Often the lifetime exceeds 100 years up to A/M ∼ 45 m²/kg, decreasing rapidly to a few months above such a threshold. However, the details of the evolution, which are conditioned by the complex interplay of solar radiation pressure and geopotential plus luni-solar resonances, depend on the initial conditions. Different behaviors are thus possible. In any case, objects like those discovered in synchronous orbits, with A/M as high as 20–40 m²/kg, could also survive in this orbital regime, with semi-major axes close to the semi-synchronous values, with maximum eccentricities between 0.3 and 0.7, and with significant orbit pole precessions (faster and wider for increasing values of A/M), leading to inclinations between 30° and more than 90°.     

Indicators of black-hole mass and Eddington accretion ratio from QSO X-ray and UV spectra

The evolution of luminous QSOs is linked to the evolution of massive galaxies. We know this because the relic black-holes found locally have masses dependent on the properties of the host galaxy’s bulge. An important way to explore this evolution would be to measure dependences of black-hole masses and Eddington accretion ratios over a range of redshifts, i.e., with cosmological age. For low redshift QSOs (and their lower luminosity Seyfert galaxy counterparts) it has been possible to infer black-hole masses from the luminosities and velocity dispersions of their host-galaxy bulges. These masses agree with those virial black-hole masses calculated from the Doppler widths of the broad Hβ emission lines. The latter method can then be extended to more distant and luminous QSOs, up to redshifts of 0.6 with ground-based optical observations. We discuss ways to extend these explorations to higher redshifts – up to 3 using the widths of QSOs’ broad UV emission lines, and in principle, and to redshifts near 4 from ground-based infrared observations of rest-frame Hβ at 2.5 μm. We discuss the possibility of investigating the accretion history of the higher redshift QSOs using measures of Eddington accretion ratio – the soft X-ray spectral index and the eigenvectors of Principal Components Analyses of QSOs’ UV emission-line spectra.