航天器上升段轨道快速重构算法

针对航天器上升飞行过程中由于干扰的影响导致实际轨道偏离初始设计轨道的问题,提出了基于状态量提前修正的航天器上升段轨道快速重构算法。使用该算法对大气干扰下上升段轨道进行了快速重构仿真分析,结果表明,该算法能够综合考虑上升段飞行过程的状态量约束、终端约束、入轨精度、重构时间等因素,实现快速重构。     

隐身等离子体的几个相关问题研究

在目标的雷达隐身方面,等离子体具有巨大的应用潜力。对隐身应用时产生等离子体的气压、放电气体种类以及放电方式进行了论述。指出在大气压下,适宜利用惰性气体放电来产生等离子体。而目前许多文献中所报道的隐身等离子体的产生方法离工程应用还有一定距离,还有许多问题亟待解决。     

光学加工射频离子源的去除函数与稳定性研究

在研究了射频离子源的结构、工作原理和性能的基础上,进行了光学镜面抛光离子束的去除效率与稳定性测试。实验结果表明射频离子源去除函数的形状为回转高斯形,利用Φ15mm的栅网,在靶距为30mm、离子能量900eV时,去除函数的峰值去除率为194nm/min,体积去除率为19.2×10-3mm3/min,半峰全宽值为9.2mm;并且去除函数的峰值去除率与体积去除率的变化均在3%以内,半峰全宽值的变化在1.7%以内。因此,射频离子源具有光学镜面抛光加工所需的去除效率,而且射频离子源具有好的稳定性,具备光学加工的潜能。     

离子推进器和流量控制单元

使用电动电源线确保使用电力,它等于几十千瓦。 建议它应该高达10000秒。 Keldysh研究中心（KeRC）正在开发推进系统。 35千瓦离子推进器和FCU-500流量控制单元。 IT-500和FCU-500的2000小时寿命测试是 离子推进器大部分运行2018小时,使用40千克氙气。 本文还介绍了磁场和离子光学的改进以及石墨网格的发展状况。     

基于主被动量子关联成像的超分辨抗干扰探测系统研制

针对大气湍流以及不同光照条件下难以成像的问题,提出了基于空间光场调制的主被动量子关联成像方案。研制了超分辨抗干扰的主被动量子关联成像原理样机,并完成了超分辨、抗大气湍流以及不同光照条件下的外场实验,验证了主被动量子关联成像原理样机的全天时抗干扰成像能力,实现了超分辨的远距离成像探测。本方案为远距离遥感、极弱背景探测提供了一种有效的成像技术手段。     

A Celestial Analytic Positioning Method by Stellar Horizon Atmospheric Refraction

This article, in allusion to the limitation of conventional stellar horizon atmospheric refraction based on orbital dynamics model and nonlinear Kalman filter in practical applications, proposes a new celestial analytic positioning method by stellar horizon atmospheric refraction for high-altitude flight vehicles, such as spacecraft, airplanes and ballistic missiles. First, by setting up the geometric connexion among the flight vehicle, the Earth and the altitude of starlight refraction, an expression for the relationship of starlight refraction angle and atmospheric density is deduced. Second, there are produced a novel measurement model of starlight refraction in a continuous range of altitudes (CRA) from 20 km to 50 km on the basis of the standard atmospheric data in stratosphere, and an empirical formula of stellar horizon atmospheric refraction in the same altitudes against the tangent altitude. Third, there is introduced a celestial analytic positioning algorithm, which uses the least square differential correction instead of nonlinear Kalman filter. The information about positions of a flight vehicle can be obtained directly by solving a set of nonlinear measurement equations. The stellar positioning algorithm adopts the characteristics of stellar horizon atmospheric refraction thereby removing needs for orbit dynamics models and priori knowledge of flight vehicles. The simulation results evidence the validity of the proposed stellar positioning algorithm.     

二维紊流场对飞艇水平面内运动影响研究

大气紊流是影响高空飞艇水平面内巡航的重要原因,传统Dryden模型采用谱分解定理,只能生成一维大气紊流模型,对于高空飞艇复杂的飞行运动来说,生成二维紊流风场模型是必要的.基于紊流场的空间相关特性,采用离散自递归方法构建风场模型,然后结合风速矢量三角形关系式,建立扰动下的飞艇动力学模型,再对该模型进行水平竖直解耦.仿真结果表明,大气紊流作用在飞艇上的力会使飞艇较大程度地偏离其运动航迹,呈不稳定的随机波动状态.因此,构建高空飞艇动力学模型时,要充分考虑大气紊流的影响.     

用于直升机在大气紊流中的旋翼状态反馈控制

发展了一种集成旋翼状态反馈(Rotor-State Feedback,RSF)控制的飞行控制系统,以提升直升机在大气紊流环境中低速飞行时的飞行品质。基于经典显模型跟踪控制系统,对机体和旋翼状态反馈增益进行协同设计,以综合优化旋翼/机体耦合动稳定性和直升机在飞行品质相关频率范围(1~12rad/s)内的紊流缓和能力。同时,设计了一个旋翼前馈控制以增强直升机的操纵响应特性。对直升机飞行品质的线性分析表明:RSF控制的引入能够在实现旋翼/机体耦合动稳定性控制的同时使滚转和俯仰通道的指令跟踪延迟时间分别降低21.87%和25.82%,扰动抑制带宽分别提升243.22%和72.56%。最后以飞行试验验证的高阶非线性飞行动力学模型进行数值模拟验证控制系统。结果表明:RSF控制的引入使直升机滚转、俯仰角速率对紊流响应的标准差分别降低55.68%和26.81%。集成RSF的控制系统能够提升直升机在紊流中的飞行品质。     

空间目标的地面光谱特性和星等估计

针对自适应光学系统将要探测的空间非自发光目标,进行了光谱特性和星等估计的研究;研究了空间非自发光目标反射太阳光穿过大气层而进入自适应光学系统的波前探测器的子孔径内的光子速率;同时还针对反射太阳光的空间目标亮度太低,研究了激光照射目标后的相应情况。     

Exploring The Saturn System In The Thermal Infrared: The Composite Infrared Spectrometer

The Composite Infrared Spectrometer (CIRS) is a remote-sensing Fourier Transform Spectrometer (FTS) on the Cassini orbiter that measures thermal radiation over two decades in wavenumber, from 10 to 1400 cm^{− 1} (1 mm to 7μ m), with a spectral resolution that can be set from 0.5 to 15.5 cm^{− 1}. The far infrared portion of the spectrum (10–600 cm^{− 1}) is measured with a polarizing interferometer having thermopile detectors with a common 4-mrad field of view (FOV). The middle infrared portion is measured with a traditional Michelson interferometer having two focal planes (600–1100 cm^{− 1}, 1100–1400 cm^{− 1}). Each focal plane is composed of a 1× 10 array of HgCdTe detectors, each detector having a 0.3-mrad FOV. CIRS observations will provide three-dimensional maps of temperature, gas composition, and aerosols/condensates of the atmospheres of Titan and Saturn with good vertical and horizontal resolution, from deep in their tropospheres to high in their mesospheres. CIRS’s ability to observe atmospheres in the limb-viewing mode (in addition to nadir) offers the opportunity to provide accurate and highly resolved vertical profiles of these atmospheric variables. The ability to observe with high-spectral resolution should facilitate the identification of new constituents. CIRS will also map the thermal and compositional properties of the surfaces of Saturn’s icy satellites. It will similarly map Saturn’s rings, characterizing their dynamical and spatial structure and constraining theories of their formation and evolution. The combination of broad spectral range, programmable spectral resolution, the small detector fields of view, and an orbiting spacecraft platform will allow CIRS to observe the Saturnian system in the thermal infrared at a level of detail not previously achieved.This revised version was published online in July 2005 with a corrected cover date.