适用于星敏感器的导航星表构造算法研究

导航星表的性能对于星敏感器姿态测量的实时性及精度至关重要。为了克服星等过滤算法的缺点,将支持向量机应用于导航星表的构造算法中。将基本星表中的恒星视为待分类的数据点,选取抽样视场中最亮的k颗星作为导航星,而非导航星的数量由抽样视场中恒星的密度决定。为了获得具有最大推广能力的抽样数据,采用了一种球面螺旋形算法生成抽样视场视轴指向,使用抽样数据构建最优导航星分类器,应用最优导航星分类器对基本星表中每一颗恒星进行分类判决。仿真结果表明,在满足8°×8°视场中至少出现3颗导航星的条件下,该算法生成的导航星表导航星总数约为星等过滤算法的33%,比传统支持向量机算法减少了7.8%,其标准差仅为星等过滤算法的21%,这表明本算法在导航星表容量及导航星分布均匀性方面大大优于星等过滤算法和传统支持向量机算法。     

激光导星角度与聚焦非等晕性综合分析

采用自适应光学(AO)系统对湍流大气进行校正时,非等晕性误差的影响不可避免。基于空间谱滤波技术,围绕湍流大气角度、聚焦、角度与聚焦相耦合非等晕性问题,进行了统一建模,给出了不同情况下的理论描述公式,分析了纯角度和纯聚焦非等晕误差中不同泽尼克模式分量所占比份。针对典型AO系统工作模式,分析了不同高度大气层对非等晕性误差的贡献。实际应用时,根据应用场景,应对AO系统工作模式和信标模式做优化匹配选择。     

激光导星角度与聚焦非等晕性综合分析

采用自适应光学（AO)系统对湍流大气进行校正时,非等晕性误差的影响不可避免。基于空间谱滤波技术,围绕湍流大气角度、聚焦、角度与聚焦相耦合非等晕性问题,进行了统一建模,给出了不同情况下的理论描述公式,分析了纯角度和纯聚焦非等晕误差中不同泽尼克模式分量所占比份。针对典型AO系统工作模式,分析了不同高度大气层对非等晕性误差的贡献。实际应用时,根据应用场景,应对AO系统工作模式和信标模式做优化匹配选择。     

Image jitter of a laser guide star in a monostatic formation scheme

The image jitter of a spherical wave with a random center is calculated. A rigorous formula is proposed for a random vector that determines the image position of the spherical wave at the focus of the telescope under the condition that the source position also fluctuates. The variance of these fluctuations is calculated. The dependence of the variance on parameters describing the optical experiment is analyzed. The analysis of this problem is of interest for solving of a number of practical tasks including the analysis of the possibility of solution of the tilt problem upon using a laser guide star.     

基于同步探测的脉冲钠导星聚焦非等晕性实验研究

本文提出在大气Greenwood时间常数内采用同步探测技术实现钠导星聚焦非等晕性测量, 开展了脉冲体制钠导星探测实验, 实现了对大气平流层顶端钠导星和同路径自然星可见光波段的哈特曼点阵的同步探测, 并获得钠导星回光单帧波面, 从波面一致性对比、Zernike系数比较、模拟成像校正等方面对实验结果进行较全面分析. 实验结果表明, 在当前实验条件下, 虽然脉冲钠导星的单帧哈特曼点阵的成像对比度较低, 制约了波面恢复精度, 但同步测量的两组波面始终能保持相似性, 其Zernike系数在前36阶一致性较好, 模拟结果表明钠导星探测波面有助于实现对自然星成像的有效校正, 扣除波面恢复误差后的聚焦非等晕性方差小于0.1 rad², 十分接近理论结果.     

Experimental validation of a technique to measure tilt from a laser guide star

We have experimentally demonstrated for what is believed to be the first time a method for sensing wave-front tilt with a laser guide star (LGS). The tilt components of wave fronts were measured synchronously from the LGS by use of a telescope with a 0.75-m effective aperture and from the star Polaris by use of a 1.5-m telescope. The Rayleigh guide star was formed at an altitude of 6 km and at a corresponding range of 10.5 km by projection of a focused beam at Polaris from the full aperture at the 1.5-m telescope. Both telescope mounts were unpowered and bolted in place, allowing us to reduce substantially the telescope vibration. The maximum value of the measured cross-correlation coefficient between the tilt for Polaris and the LGS is 0.71. The variations of the measured cross-correlation coefficient in the range from 0.22 to 0.71 are caused by turbulence at altitudes above 6 km, which was not sampled by the laser beacon but affected tilt for Polaris, the cone effect for turbulence below 6 km, residual mount jitter of the telescopes, and variations of the signal/noise ratio. The results support our concept of sensing atmospheric tilt by observing a LGS with an auxiliary telescope and indicate that this method is a possible solution for the tip-tilt problem.     

Construction and evaluation of embedding functions

Non-self-consistent density functional theories require specification of the embedding energy for an atom in a reference system. We combine the embedding energies determined from linear muffin tin orbital (LMTO) calculations of the bulk cohesive energy curves with those determined from the experimental diatomic binding curve. These new embedding functions contain information about the variation of binding with both coordination and separation between atomic centers. These are shown to be superior to embedding functions determined solely from bulk cohesive energy curves through tests on structures and energies of small metal clusters, self-diffusion of adatoms on metal surfaces, and scattering of metal atoms from metal surfaces.     

Performance evaluation of 16 channel DWDM radio-over-fiber link

In this article, generation of DWDM-RoF signal utilizing an SOA-MZI multichannel frequency up-conversion is demonstrated. The simulation results of a 16 channel, 10 km DWDM-RoF link at baseband signal of 500 Mbps, over the wavelength range 1545.80–1552.20 nm are reported. BER of the order of e⁻¹⁸ and Q factor above 18 dB over the entire bandwidth signify negligible crosstalk and error free transmission of radio signal.     

Hypernuclear fine structure in (16)(Lambda)O and the LambdaN tensor interaction

We have observed two gamma-ray transitions in (16)(Lambda)O from the 6.6 MeV excited 1(-)(2) state to both ground-state spin-doublet members (1(-)(1),0(-)) by the (K-,pi(-)gamma) reaction. We have obtained the ground-state doublet spacing to be 26.4+/-1.6(stat)+/-0.5(syst) keV and the excitation energy of the 1(-)(2) state to be 6561.7+/-1.1(stat)+/-1.7(syst) keV. The ground-state doublet spacing provides a small but nonzero strength of the tensor interaction between a Lambda and a nucleon. This is the first experimental result on the LambdaN tensor interaction.     

Microscopic scattering imaging measurement and digital evaluation system of defects for fine optical surface

According to ISO10110-7 and the engineering standards of Inertial Confinement Fusion (ICF), this paper presents a microscopic scattering imaging and analyzing system which allows one to automatically evaluate defects in random distributions and shapes on the surface of fine optical components of large aperture. The annularly disposed multi-beam fiber light sources illuminate the target surface with a special angle. The image, which has bright defects on black background, is suitable for digital image processing. With XY-scanning system, the defect information of full aperture can be obtained by stitching the sub-aperture image array, according to the algorithms of template matching. The full aperture image is divided into N × N sub-apertures, each of which has view field of approximate 3 mm × 4 mm. Image processing software for image recognition has been established using mathematical morphology with high computing efficiency and friendly graphics user interface. A group of standard reticules fabricated by binary optics can scale defects for calibration. As a result the lateral resolution of the system is better than sub-micrometer while the total view field can be hundreds of millimeters. The comparison quantitative data results between the experiment and standard demonstrate the system is competent for the digital evaluation of defect characterization of fine optical surfaces, especially for the ones with large aperture.