飞机突防飞行非线性解耦控制系统的混合仿真研究

飞机低空突防作地形跟踪／回避飞行时，会出现纵向和横向运动的非线性交叉耦合，利用非疆性逆系统理论和现代最优控制理论可以设计一个飞行控制规律来解开这些耦合，主要讨论了这种线性解耦控制系统的混合仿真，给了用于仿真的数学模型以及仿真方法，对系统有无大气紊流扰动的解耦控制、系统对指令输入的跟踪、飞行品质等方面进行了探讨。结果表明，该控制规律在有无大气紊流影响时都能实现解耦，准确地跟踪期望的三维突防航迹，并具     

Time series analysis of active galactic nuclei: The case of Arp 102B, 3C 390.3, NGC 5548 and NGC 4051

We used the Z-transformed Discrete Correlation Function (ZDCF) and the Stochastic Process Estimation for AGN Reverberation (SPEAR) methods for the time series analysis of the continuum and the Hα$\alpha$ and Hβ$\beta$ line fluxes of a sample of well known type 1 active galactic nuclei (AGNs): Arp 102B, 3C 390.3, NGC 5548, and NGC 4051, where the first two objects are showing double-peaked emission line profiles. The aim of this work is to compare the time lag measurements from these two methods, and check if there is a connection with other emission line properties. We found that the obtained time lags from Hβ are larger than those derived from the Hα analysis for Arp 102B, 3C 390.3 and NGC 5548. This may indicate that the Hβ   line originates at larger radii in these objects. Moreover, we found that the ZDCF and SPEAR time lags are highly correlated (r∼0.87$r\sim 0.87$), and that the error ranges of both ZDCF and SPEAR time lags are correlated with the FWHM of used emission lines (r∼0.7$r\sim 0.7$). This increases the uncertainty of the black hole mass estimates using the virial theorem for AGNs with broader lines.     

资料转移技术在三维有限元中的应用

本文研究了两类用于三维h自适应网络管理的资料转移方法。文中将牺牲解的精度以节省计算时间的一类资料转移的简单方法（简法）与另一类在资料转移中确保解决的精度的严格方法（严法）进行了比较分析，并通过数值计算例题进行了论证，结果表明：对于简单问题，两类方法都能满足精度，完成资料转移。对于复杂应力状态问题，严法可靠，特别是在网络稀疏时，严法明显优越。     

对偶变换及其在冗余度机器人中的应用

给出了用对偶数矩阵来描述冗余度机器人的雅可毕方程的方法，对偶阵及其变换是这一方法的基础，对偶阵方法可使机器人节点参数的描述变得简洁，尤其在可毕矩阵的直接确定过程中这一方法更显得有效，对偶变换这一方法对机器人运动学、动力学、控制系统之建模提供一种简化的有效方法。     

CAPP系统中工艺路线生成研究

本文研究ＣＡＰＰ中回转体类零件在工序组合之后，确定各工序间的前趋和后继关系，建立拓扑排序的ＡＯＶ网，并由此形成工艺路线的方法。     

铬白口铸铁中硅对组织形态的影响

本文采用高硅进行白口铸铁的合金化。实验发现，随着硅含量的增加，碳化物形貌由网状向断网状、直至分散孤立的条块状变化，碳化物的含量逐渐增加，碳化物的尺寸细化，碳化物硬度、基体硬度也逐渐增大。当硅量〉２．５％，铬量〉５％时，组织中出现了Ｍ７Ｃ３。     

Active galactic nuclei imaging programs of the RadioAstron mission

Imaging relativistic jets in active galactic nuclei (AGN) at angular resolution significantly surpassing that of the ground-based VLBI at centimetre wavelengths is one of the key science objectives of the RadioAstron space-VLBI mission. There are three RadioAstron imaging key science programs that target both nearby radio galaxies and blazars, with one of the programs specifically focusing on polarimetry of the jets. The first images from these programs reach angular resolution of a few tens of microarcseconds and reveal unprecedented details about the jet collimation profile, magnetic field configuration, and Kelvin-Helmholtz instabilities along the flow in some of the most studied AGN (3C 84, BL Lac, 3C 273, S5 0836 + 710). Here we give an overview of the goals and strategy of these three ongoing programs, highlight their early results, and discuss the challenges of space-VLBI imaging.     

Off-axis irradiation and the polarization of broad emission lines in active galactic nuclei

The stokes Monte Carlo radiative transfer code has been extended to model the velocity dependence of the polarization of emission lines. We use stokes to present improved modeling of the velocity-dependent polarization of broad emission lines in active galactic nuclei. We confirm that off-axis continuum emission can produce observed velocity dependencies of both the degree and position angle of polarization. The characteristic features are a dip in the percentage polarization and an S-shaped swing in the position angle of the polarization across the line profile. Some differences between our stokes results and previous modeling of polarization due to off-axis emission are noted. In particular we find that the presence of an offset between the maximum in line flux and the dip in the percentage of polarization or the central velocity of the swing in position angle does not necessarily imply that the scattering material is moving radially. Our model is an alternative scenario to the equatorial scattering disk described by Smith et al. (2005). We discuss strategies to discriminate between both interpretations and to constrain their relative contributions to the observed velocity-resolved line and polarization.     

基于刷扫和研磨的复合式小行星取样器取样过程仿真与分析

针对小行星表面微重力环境及样品机械属性未知的特点,提出了一种基于刷扫和研磨的复合式取样器设计方案。该取样器通过刷扫和研磨的复合方式进行取样,能够提高小行星表面取样任务的成功率。为了研究该取样器刷扫取样时刷轮叶片数、刷轮转速、推进速度、星壤参数等对取样效率的影响,研磨和刷扫复合取样的优越性以及刷扫和研磨时的驱动力矩,开展了样品颗粒相互作用建模及研磨取样动力学分析。基于离散元仿真软件EDEM,构建了取样器3D模型并仿真其在小行星表面取样,获得了样品收集质量与取样时间的关系曲线,分析了各个参数对取样效率的影响。结果表明:刷轮叶片数越多,刷轮转速越大,推进速度越大,取样器取样效率更高,刷扫和研磨的复合取样方法比起单一的刷扫取样,具有更高的取样效率。该研究为设计小行星取样器、取样参数设定和取样效果分析提供了依据。     

Efficiency tests for estimating the gas and stellar population parameters in Type 2 objects

We investigated the efficiency of estimating characteristics of stellar populations (SP) and Active Galactic Nuclei (AGN) emission using ULySS code. To analyze simultaneously AGN and SP components in the integrated spectrum of Type 2 active galaxies, we modeled the featureless continuum (FC) and emission lines, and we used PEGASE.HR stellar population models provided by ULySS. In order to validate the method, we simulated over 7000 integrated spectra of Seyfert 2 galaxies. Spectra were generated using different characteristics of the featureless AGN continuum, signal-to-noise ratio (SNR), spectral ranges, properties of emission lines and single stellar population (SSP) model whose initial mass function (IMF) and abundance pattern is similar to the solar neighborhood. Simulated spectra were fitted with ULySS to evaluate the ability of the method to extract SP and AGN properties. We found that the analysis with ULySS can efficiently restore the characteristics of SP in spectra of Seyfert 2 AGNs, where signal-to-noise ratio is higher than 20, and where SP contributes with more than 10% to the total flux. Degeneracies between AGN and SP parameters increase with increasing the AGN continuum fraction, which points out the importance of simultaneous fitting of the FC and SP contributions.