土星探测器飞行动力学与轨道计算

根据牛顿第二定律和万有引力定律，建立了空间探测器的运动微分方程，并以土星探测器为例，利用精确的数值积分方法对其轨道进行了设计和计算，在土星探测器的轨道设计和计算中，充分利用了有关天体的引力机动，有目的地使探测器飞过一系列行星来增加探测器的能量，从而大大降低了探测器的发射条件。     

Hubble Space Telescope spectroscopy of massive hot stars in the Magellanic Clouds and M31

Using the Hubble Space Telescope (HST) and the Faint Object Spectrograph (FOS) high signal to noise spectrograms were obtained for 15 OB stars in the Magellanic Clouds^***, three of which are of spectral type O3. The data cover the spectral region from 1150 A – 2300 A with a resolution of /1 A. One O8.5 supergiant, OB78#231, in M31is also included in this work. These data are a substantial improvement on previous high resolution IUE observations in the Magellanic Clouds (Walborn et al. 1985 and references therein) because of the smaller aperture and the much better signal to noise ratio, while no high resolution UV spectra of O stars in M31 have been obtained before. In this paper we discuss various morphological aspects of the spectra, concerning metallicity and the stellar winds, compared to galactic analogues.     

Analysis of a redshifted plasma flow over a sunspot

The ultraviolet spectrum of a redshifted plasma flow appearing over a sunspot observed during the first flight of the High Resolution Telescope Spectrograph (HRTS I) is analysed, and interpreted as a radiatively cooling plasma. For most of the lines emitted from this plasma, the assumption of ionization equilibrium during the cooling is good. However for He II (and other ions with a single electron outside of closed shells), this is not the case. Integrating differential equations for the various ionization fractions of helium and the temperature allows an approximate determination of the abundance of helium relative to other elements whose lines appear in the spectrum of the plasma flow.     

Electron coronal density irregularity\overline {n^2 } /(\bar n)^2 from measurements of K-coronal and lyman lines brightnesses

We propose a technique to derive the coronal density irregularity factor , wheren is the electron density. The absolute photometric comparison between the intensity of UV lines and the white-light K-coronal polarized brightness (pB) provides an unique constraint on the inhomogeneity of the corona. The ratio of the measured H I Lyman (Ly-) line intensity to the resonant-scattering dominated H I Lyman (Ly-) intensity can be used to extract the collisonal component of the Ly-. This component yields an estimate of . The quantity is then obtained from white-light K-coronal measurements. The use of lines of the same atomic species minimizes the effects due to outflow velocities (i.e., Doppler dimming), and reduces the errors introduced by the uncertainties in the ionization balance, the atomic parameters, and the solar abundances. The UVCS/SOHO unique capability of performing cotemporal and cospatial measurements of the Ly- and Ly- lines, and ofpB makes this instrument ideal for implementing this technique.     

一种频分制遥测系统的设计与研制

介绍了某战斗弹上所用的频分制遥测系统。对该系统的遥测参数及遥测系统主要指标进行了分析，并介绍了研制中解决的主要关键技术问题     

实测数据的降秩空时自适应处理方法

在实际非均匀环境中，机载雷达数据的非均匀性会恶化杂波协方差矩阵的估计，严重地降低了空时自适应处理器的性能。本文首先用非均匀检测器在非均匀环境下选择辅助距离门，来估计样本协方差矩阵。而后讨论了基于广义旁瓣相消器结构上的两种降秩空时自适应处理方法：主分量法和互谱法，这两种方法都是利用杂波和干扰的低秩属性，用依赖于采样数据的转换矩阵来构造空时自适应滤波器。最后对从Mountain Top计划测得的数据，应用上述两种降秩方法对其进行了分析。仿真实验表明了这两种方法的可行性，减少了计算量，并提高了有效可测收敛性，可有效地提高空时自适应处理器的性能。     

基于计算机视觉任务的图像直线提取技术

提出一种基于计算机视觉任务的图像直线提取技术 ,首先用边界检测算子提取边缘 ,然后用链码将边缘表示出来 ,并记录链码的端点 ,即直线的端点 ,通过逐步删除对计算机视觉任务无意义的链码 ,得到图像直线的链码表示 ,最后用最小二乘法拟合图像直线的链码。该技术能尽可能多地从图像中提取直线信息 ,既可以较准确地提取直线的端点信息 ,又能得到直线的准确表示     

用于PolyStrata技术的光刻工艺探索研究

在高集成的射频微机电系统RF MEMS（Radio Frequency Micro Electro Mechanical System）器件的发展趋势下，三维集成工艺的研究越来越多。基于PolyStrata技术的三维多层堆叠同轴器件以其无色散、低损耗、超宽带的优势脱颖而出，PolyStrata技术使用紫外厚胶作为牺牲材料，对光刻胶粘附性、精度、工艺兼容及释放性能要求高，常规厚胶难以满足。探索A、B两种紫外光刻厚胶，对两者工艺参数及图形质量进行对比研究。结果表明，光刻胶A厚度均匀性为98.6%，图形偏差小于10μm；光刻胶B图形偏差小于5μm，但均匀性较差，约80.4%。     

The spatial distributions of the sources of UV solar Explosive Events at different velocities

We analyze five solar Explosive Events observed in the Si iv emission line at 139.37 nm during SUMER/SoHO raster scans near disk center. The Doppler velocities from −45 km s⁻¹ to +45 km s⁻¹ were sorted into eleven symmetrically organized velocity bins, five equally-sized bins on each side and one bin for the line at rest. The radiance values along the NS oriented slit around the maximum of each EE are used to build one-dimensional distributions. We study these distributions and their development in space and time for different velocity bins to unveil the 3D-structure and evolution of Explosive Events. The spatial radiance distributions for the EE maximum and around it were made. For some Explosive Events the dispersion direction is not oriented orthogonally to the slit direction; consequently, the blueshifted emission is in a linear way offset from the redshifted emission by several pixels. The largest offset (∼5″) is observed between distributions whose velocities differ by ∼36 km s⁻¹. The linear relation agrees with an scenario of flows inside magnetic arcs.     

Synthesis,chemistry and photochemistry of cyanobutadiyne (HCCCCCN)

Cyanobutadiyne has been synthesized starting from the mono or bistributylstannyl derivative of 1,3-butadiyne and p-toluenesulfonyl cyanide. The UV spectrum of HC₅N and the ¹³C NMR spectrum of the deuterocyanobutadiyne DC₅N have been recorded for the first time. Cyanobutadiyne has been detected in the photolysis of mixtures of gases observed on Titan. Its formation starting from cyanoacetylene and acetylene also occurs in the presence of huge amounts of dinitrogen, the major constituent of the Titan’s atmosphere. The application of these findings to the atmosphere of Titan is discussed. The chemistry and photochemistry of cyanobutadiyne have been investigated. A photoadduct has been observed in the photolysis of cyanoacetylene and ethanethiol and, a univocal synthesis of this compound was performed by a nucleophilic addition reaction.