基于神经网络的SINS/GPS/TAN 容错组合导航系统设计

在联邦滤波器结构的基础上 ,设计了一种基于神经网络的天文惯性导航系统 /全球卫星定位系统 /战术导航系统 (SINS/GPS/TAN)容错组合导航系统。该系统首先在各子滤波器中用神经网络滤波 (NNF)代替传统的卡尔曼滤波 ,然后用模糊神经网络 (FNN)对各子系统进行故障检测 ,最后由神经元进行全局融合。通过仿真 ,验证了该方法的有效性     

Wolf–Rayet optically thick winds with Alfvén waves

The Wolf–Rayet (WR) stars are hot luminous objects which are suffering an extreme mass loss via a continuous stellar wind. The high values of mass loss rates and high terminal velocities of the WR stellar winds constitute a challenge to the theories of radiation driven winds. Several authors incorporated magnetic forces to the line driven mechanism in order to explain these characteristics of the wind. Observations indicate that the WR stellar winds may reach, at the photosphere, velocities of the order of the terminal values, which means that an important part of the wind acceleration occurs at the optically thick region. The aim of this study is to analyze a model in which the wind in a WR star begins to be accelerated in the optically thick part of the wind. We used as initial conditions stellar parameters taken from the literature and solved the energy, mass and momentum equations. We demonstrate that the acceleration only by radiative forces is prevented by the general behavior of the opacities. Combining radiative forces plus a flux of Alfvén waves, we found in the simulations a fast drop in the wind density profile which strongly reduces the extension of the optically thick region and the wind becomes optically thin too close its base. The understanding how the WR wind initiate is still an open issue.     

利用星敏感器的卫星自主导航

本课题对利用星敏感器进行卫生自主导航问题作了初步的研究，研究表明，当已知地球大气的星光折射模型，则可利用星光折射的测量或掩星时刻的测量来实现卫生的自主导航，在导航过程中不需要精确的姿态确定，研究报告提出了相应的基本导航算法，讨论了误差的影响，通过数学仿真模拟计算，给出了数值结果，提示了这类导航的若干特点。     

Macroscopic Transport Large-scale advection, turbulent diffusion, wave transport

While the solar convection zone is very well mixed by its turbulent motions, chemical composition gradients build up in the radiative interior due to microscopic diffusion and settling, and to nuclear burning. Standard models, which ignore any type of macroscopic transport, cannot explain the depletion of lithium in solar-type stars, as they evolve; neither do they account for the observed profile of molecular weight at the base of the solar convection zone. Such macroscopic transport can be achieved through thermally driven meridian currents, through turbulent diffusion generated by differential rotation and possibly through gravity waves. These processes transport also angular momentum, and therefore the internal rotation profile of the Sun provides a crucial test for their relative importance. So does also the behavior of tidally locked binaries, which appear to destroy less lithium than single stars of the same mass. This revised version was published online in June 2006 with corrections to the Cover Date.     

星光折射连续修正方法及制导规划

针对星光折射模型本身固有的缺点，对星光折射连续修正方法进行了研究，该方法首先探索折射星的分布规律，而后采用Unscented卡尔曼滤波算法+多星连续观测的方案实现定位。同时，对可用星与选星要素和基于突防规划的星光制导弹道设计两方面进行了研究，在星光制导制约机理研究的基础上，提出了惯性/星光制导规划方法，该方法包括导航星的优选策略、导航星优选技术和星点位置的精确计算3步。最后，介绍了星光制导系统的系统组成和功能原理。     

Evidence of Element Diffusion Inside the Sun and the Stars and its Consequences on the Lithium Primordial Abundance

The process of element segregation in stars (also called "microscopic diffusion") has to be introduced in all computations of stellar structure to obtain consistent models. Although recognized by the pioneers of stellar physics, this process has long been forgotten, except for white dwarfs and for the so-called "chemically peculiar stars". More recently helioseismology has given evidence that this process occurs in the Sun, and leads to helium and heavier element depletion by about 20 percent. Some macroscopic motions (mild mixing) must also occur below the convection zone in order to account for the lithium depletion. These motions do not prevent the segregation : they only slightly smooth the abundance gradients. These results are presented here and the connexion with the 3He abundance is discussed. The importance of these processes for Pop II stars is also developped.     

The synthesis of helium and CNO isotopes in massive stars

We present helium and CNO isotopic yields for massive mass-losing stars in the initial mass range 15M M _i 50M . We investigate their dependence on assumptions about mass loss rates, internal mixing processes, and metallicity, and specify the contributions from stellar winds and from supernova ejecta.     

远场假设对喷流噪声预测中格林函数求解的影响

目前基于雷诺平均Navier-Stokes（RANS）的喷流噪声预测方法在格林函数求解时, 为简化求解过程,通常对喷流流动做平行流假设, 对观测点做远场假设。随着格林函数求解方法发展,近年来的研究表明平行流假设对下游观测点格林函数的计算会引起较大偏差,而目前远场假设对格林函数求解的影响仍不清楚。为研究远场假设对喷流格林函数求解的影响,以二维喷流为例, 采用计算气动声学方法（CAA）分别数值求解了观测点远场假设条件与实际条件下90°~150°方向喷流内伴随格林函数,进而分析远场假设对格林函数求解的影响。研究结果表明,对于不同方向的观测点,由观测远场假设导致的伴随格林函数求解偏差不尽相同,且对于越靠近喷流中心线方向的观测点,远场假设导致的偏差越大,其中150°方向观测点,采用远场假设后,格林函数计算结果最大偏差达到-15 dB以上。因此,对于靠近喷流中心线方向的噪声观测点而言,为避免预测偏差,应采用实际观测条件求解喷流格林函数。     

激波冲击下Air/SF6斜界面不稳定性实验研究

激波在不同密度介质上的交互作用在可压缩湍流上具有重要的基础价值。激波在界面上的作用会引起Richtmyer-Meshkov不稳定性。激波不正规折射时,流场存在更多复杂的涡。研究马赫数为1.23、1.41的激波在初始倾角β=60°的Air/SF6界面上非正规折射的情况。入射激波的切向冲击和法向冲击的相互作用,在界面处产生涡,折射波在壁面发生马赫反射。利用阴影显示技术,给出了界面演化和混合的过程。     

机匣视窗折射对LDV聚焦的影响分析

为了分析激光束经过机匣视窗后聚焦状态的变化情况, 发展了一套通用程序, 可用于计算不同的测量条件下, 激光束穿过不同尺寸机匣视窗时的折射情况, 并对其结果的可信性进行了验证.利用所发展的程序, 以二维LDV探头为例, 分析了典型情况下蓝光、绿光焦点偏移情况, 以及蓝光与绿光焦点之间偏移量的变化情况, 并给出了确定焦点重合的计算准则.计算结果表明:如果不进行特殊的光学修正, LDV测量时必须要选取小的探头角度和浅的测点深度.