超声速隐身歼轰机概念设计数值模拟

为了提高军用飞机的空战和对面攻击能力,对歼轰机进行总体设计。采用CATIA软件,设计出隐身歼轰机的三维数字样机和武器挂载方案;基于物理光学法和等效电磁流法,采用自编的RCSAnsys软件,数值模拟歼轰机的数字样机在X、S和UHF波段下的RCS特性和强度分布特性;基于湍流模型的k-ε方程和控制理论的N-S方程,采用Fluent软件,数值模拟歼轰机的数字样机所在空气流场的压强和速度分布云图,得出整机的升阻特性。概念设计数值模拟结果表明：内置弹舱的歼轰机前向±30°的RCS均值≤-4.728 dBsm,超声速飞行时歼轰机的升阻比约等于5.6337。     

空间平台发射拦截器动力学与最优脉冲拦截

研究了空间平台发射拦截器的两体耦合动力学,以及拦截器拦截目标星的最优脉冲控制问题。平台首先与目标星形成绕飞关系,保持其发射筒轴线始终瞄准目标星。接到发射指令后,拦截器从发射筒中射出,本文采用拉格朗日第二类方程建立了发射过程平台-拦截器两体动力学模型。因为两体耦合影响,平台姿态偏转,拦截器出筒时的速度已经不能瞄准目标星。通过小型火箭发动机给其施加速度脉冲,使其进入拦截轨道,保证拦截的同时,将脉冲速度最小化以节省燃料,本文将其归结为一个非线性规划问题,采用三级优化的策略来求解。在拦截飞行时间相较于平台绕飞目标星的周期是小量的条件下,可以视绕飞平均角速度为小参数,采用正则摄动方法求出非线性规划的一阶近似解,然后以此为迭代初值,寻找最优真解。最后进行了数值仿真验证。     

航天器轨道追逃博弈多阶段强化学习训练方法

针对航天器轨道追逃博弈问题,提出一种多阶段学习训练赋能方法,使得追踪星在终端时刻抵近逃逸星的特定区域,而逃逸星需要通过轨道机动规避追踪星。首先,构建两星的训练策略集,基于逻辑规则设计追踪星和逃逸星的机动策略,通过实时预测对方的终端位置,设计己方的期望位置和脉冲策略,显式给出追逃策略的解析表达式,用于训练赋能;其次,为提升航天器的训练赋能效率及应对未知环境的博弈能力,提出一种基于强化学习技术多模式、分阶段的学习训练方法,先使追踪星和逃逸星分别应对上述逻辑规则引导下的逃逸星和追踪星,完成预训练;再次,开展二次训练,两星都采用邻近策略优化(PPO)策略进行追逃博弈,在博弈中不断调整网络权值,提升决策能力;最后,在仿真环境中验证提出的训练方法的有效性,经过二次训练后,追踪星和逃逸星可有效应对不同策略驱动下的对手,提升追逃成功率。     

Modeling Multifractality of the Solar Wind

The question of multifractality is of great importance because it allows us to investigate interplanetary hydromagnetic turbulence. The multifractal spectrum has been investigated with Voyager (magnetic field) data in the outer heliosphere and with Helios (plasma) data in the inner heliosphere. We use the Grassberger and Procaccia method that allows calculation of the generalized dimensions of the solar wind attractor in the phase space directly from the cleaned experimental signal. We analyze time series of plasma parameters of the low-speed streams of the solar wind measured in situ by Helios in the inner heliosphere. The resulting spectrum of dimensions shows a multifractal structure of the solar wind attractor. In order to quantify that multifractality, we use a simple analytical model of the dynamical system. Namely, we consider the generalized self-similar baker’s map with two parameters describing uniform compression and natural invariant measure on the attractor of the system. The action of this map exhibits stretching and folding properties leading to sensitive dependence on initial conditions. The obtained solar wind singularity spectrum is consistent with that for the multifractal measure on the weighted baker’s map.     

航天飞机系统两体分离问题的探讨

本文简要地叙述了美国研究轨道器与外挂贮油箱,轨道器与载机分离问题的概况。对垂直起飞两级入轨的并联两机的分离问题,提出了研究模型并作了具体分析,着重提出了实现两机安全分离需要解决的技术难点。 二级航天飞机的两机分离问题,是未来航天高技术领域的关键技术之一,本文阐述了解决两体并联分离问题我国现有的技术水平,并提出了解决该问题的技术方案。     

热流限制下的最优气动力辅助变轨

以变轨能量消耗最小为优化目标，应用极大值原理研究了飞行过程受热流限制和升力系统约束下的气动力辅助共面变轨问题，飞行过程成分第一自由弧段，约束弧段，第二自由弧段三个部分，讨论了升力系数的最优表达式，分析了飞行过程中两种约束的相互作用，给出了约束弧起始位置的角点条件和终端的横截条件下，对不同的初值选取方法讨论了三种计算策略，并给出了数值算例。     

PC-index fluctuations and intermittency of the magnetospheric dynamics

One minute resolution Polar Cap (PC) index was used for the analysis of magnetospheric dynamics. The 1995–2000 time series analysis revealed that the power spectrum of the PC-index fluctuations is a power law in a wide range of frequencies. However, the obtained exponents differ for low and high frequency regions. The probability distribution functions of the PC-index fluctuations show a strong non-gaussian shape, depending on the time of increment. This indicates that the PC-index exhibits intermittency, previously detected in solar wind and auroral electrojet index fluctuations. The PC-index probability distribution functions were fitted by the functional form proposed by Castaing et al. [Velocity probability density functions of high Reynolds number turbulence. Physica D. 46, 177–200, 1990] to describe intermittency phenomena in ordinary turbulent fluid flows. The agreement between the fitting parameters obtained for the PC index and those reported before for solar wind magnetic field fluctuations is within 30%; which is noticeably less than the difference between the same parameters of solar wind and the AE-index fluctuations. This fact indicates that the PC index reflects the solar wind influence on the high-latitude magnetosphere, especially during the summer.     

Dynamics and Composition of Rings

Planetary rings are found around all four giant planets of our solar system. These collisional and highly flattened disks exhibit a whole wealth of physical processes involving dust grains up to meter-sized boulders. These processes, together with ring composition, can help understand better the formation and evolution of proto-satellite and proto-planetary disks in the early solar system. The present chapter reviews some fundamental aspects of ring dynamics and composition. The forthcoming exploration of the Saturn system by the Cassini mission will bring both high resolution and time-dependent information on Saturn’s rings.     

The Changing Face of Titan’s Haze: Is it all Dynamics?

Titan’ atmosphere shows some similarities with that of the Earth, in terms of composition and surface pressure. Also, its seasonal cycle is similar, as Titan’ obliquity is about 27^°(23^°,5 for the Earth), although it is about 30 times as long. Titan’ haze exhibits an albedo contrast (NSA for North-South Asymmetry) that is changing seasonally. From the analysis of Voyager and Hubble Space Telescope data, we learned that at short visible wavelengths, the albedo of the winter hemisphere is lower by 10-20% than that of the summer hemisphere. This asymmetry peaks at 450 nm and reaches maximum amplitude around Titan’ equinoxes. It reverses in about five years, faster than a season which spans seven years. At longer wavelengths, longward of 700 nm, the asymmetry is inverted. The NSA reversal process in the red and in the UV seems to lead the reversal in the blue by 1 or 2 years. No valid explanation exists for this lag, at least in the red. The results from a recent model which couples atmospheric dynamics, haze microphysics and transport, as well as photochemistry, show that the NSA and its seasonal changes can be explained by an accumulation of haze particles at the winter pole. This is due to the pole-to-pole Hadley circulation pattern that is present during most of Titan’ year and rapidly disrupts at the time of the equinoxes. This model can also explain the observed cooler stratospheric temperatures and higher abundances of heavy hydrocarbons and nitriles in the winter polar region. In addition, it provides a mechanism for the formation of a detached haze layer around 300–400 km altitude, as well as the existence of a polar hood. Thus, it appears that the latitudinal contrasts we observe on Titan are conveniently tracing for us the dynamical behavior of its atmosphere.     

A systematic approach to nonlinear rotorcraft model identification

The development of a powerful parameter estimation routine and its integration into the simulation environment HOST is described. With this tool approaches are being made towards new strategies of mathematical modeling, aimed at providing highly accurate and nevertheless run-time efficient simulation models. The identification routine is capable of optimizing parameterized models in both dynamic time domain simulation and static (e.g. trim state variation) conditions. Examples of both cases are presented to emphasize the improvement in the system response prediction and to demonstrate the abilities of the identification techniques in combination with the nonlinear simulation platform. This article reviews the activities and achievements accomplished by the DLR Institute of Flight Research and the ONERA Systems Control and Flight Dynamics Department during the last few years in the research on rotorcraft flight dynamics modeling and model identification. Future activities that require extensive high fidelity modeling are in the scope of the current and coming modeling activities that include the use of the presented methods and software technologies.