宽带多媒体通信卫星多波束覆盖国土的优化研究

覆盖和染色方案的确定是研究多波束通信的前提。通过研究中国大陆区域的六边形覆盖和频率分配(染色)问题。根据建立的覆盖模型和分析,利用MATLAB提供的函数和地图信息设计了覆盖求解算法,解决了覆盖问题,并给出了染色方案。最后对进一步研究提出了展望。     

MEWMA控制图ARL计算及参数优化

平均运行链长(ARL)是控制图性能评价的一个重要指标,深入研究ARL是控制图参数优化、性能评价和实际应用的重要工作.在采样数据标准化处理的基础上,应用马尔可夫链进一步研究了多元指数移动平均(MEWMA)控制图中ARL计算的数学模型,采用Matlab实现了算法,就算法的收敛性及计算结果进行分析.以ARL为优化指标,给出了MEWMA控制图参数优化的具体步骤、计算实例和参数优化结果.      

静电悬浮加速度计控制器设计分析

对静电悬浮加速度计控制器的设计进行了详细的理论分析,得出了加速度计控制系统稳定时,必须满足的加速度计电容极板和检验荷载的距离参数、电极板面积参数、电压参数与检验荷载的质量以及气体阻尼系数与控制器参数之间的关系式,并进行了计算机仿真试验,证明该关系式是正确的,可用于静电悬浮加速度计控制器分析设计。     

高雷诺数下跨声速自然层流短舱优化设计

为解决高雷诺数下大涵道比发动机自然层流短舱高维优化设计问题,提取短舱3个基准面实现轴对称自然层流优化设计。通过获得较大范围层流区域,从而降低短舱表面摩擦阻力。采用类别形状函数（CST）参数化、γ-Re_θt转捩模型和遗传算法建立自然层流（NLF）短舱自动优化流程。表明通过优化短舱基准面建立三维NLF短舱设计方法的可行性。进而通过CATIA二次开发构建三维非轴对称NLF短舱,解决了基准面优化后大量数据点的高效导入和曲面生成问题。针对设计的非轴对称NLF短舱,进行了设计点附近迎角、侧滑角、来流马赫数以及湍流度的转捩敏感性分析。结果表明:跨声速状态下,迎角增大层流范围减小;来流马赫数增大层流范围扩大;侧滑角和湍流度对层流范围影响很小。      

6061铝合金焊后氧化物的激光清洗机理和工艺研究

采用纳秒脉冲激光器对6061铝合金焊后氧化物进行激光清洗实验。首先分析焊斑清洗前和清洗后的表面形貌和元素组成,探明焊后氧化物组成成分。其次再利用前期实验所获得不同工艺参数对清洗质量的影响规律,设计正交实验,划定各因素区间范围,分析参数对清洗质量的影响权重。利用正交实验法分析得到：影响表面轮廓线峰谷值的参数主次顺序为激光功率>脉冲频率>扫描速度>脉冲宽度;影响氧元素质量百分比的参数主次顺序为脉冲宽度>扫描速度>激光功率>脉冲频率。通过综合平衡法最终获得优化工艺参数组：扫描速度、激光功率、脉冲频率、脉冲宽度分别为2 950 mm/s、141 W、29 kHz、330 ns。优化后可确保铝合金焊后氧化物清洗彻底、无基材损伤、清洗效率高。     

单轴飞轮故障时的小卫星姿态控制方法研究

反作用飞轮和磁力矩器是现代小卫星姿态控制的主要执行机构,针对单轴反作用飞轮故障仅能提供两轴控制力矩的情况,提出了一种使用磁力矩器和反作用飞轮进行联合控制的算法。首先推导了一种拟PD姿态控制律,在此基础上提出了剩余两反作用飞轮和磁力矩器的控制力矩分配策略。仿真结果表明,该算法能够在单轴飞轮故障情况下完成小卫星高精度姿态控制任务,延长航天任务寿命,算法鲁棒性好,设计简单且易于在轨实时计算。     

Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries

Massive stars, at least \(\sim10\) times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy.In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense “clumps”. The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution.Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray sources in the sky. A large number of them consist of a neutron star accreting from the wind of a massive companion and producing a powerful X-ray source. The characteristics of the stellar wind together with the complex interactions between the compact object and the donor star determine the observed X-ray output from all these systems. Consequently, the use of SgXBs for studies of massive stars is only possible when the physics of the stellar winds, the compact objects, and accretion mechanisms are combined together and confronted with observations.This detailed review summarises the current knowledge on the theory and observations of winds from massive stars, as well as on observations and accretion processes in wind-fed high mass X-ray binaries. The aim is to combine in the near future all available theoretical diagnostics and observational measurements to achieve a unified picture of massive star winds in isolated objects and in binary systems.     

IMPROVEMENTS IN HIDDEN LINE REMOVAL ALGORITHM FOR BI PARAMETRIC SURFACES

近些年来,随着计算机图形学,计算几何和计算机辅助设计与制造技术的发展,双参数曲面的消隐算法变得越来越重要。而现有的一些消隐算法,它们在计算量,存贮量和精度上都不太令人满意。本文引入面积坐标进行包含性检验,提出移动包围盒技术,给出了一种通用性强,贮存量小,准确性高,简单快速且易于在微机上实现的消隐算法。本文还给出了由Ｄｘｙ－８８０绘图仪绘制的多个实例效果。     

EFFECTS OF INHALED TiO2 NANOTUBES ON LUNG TISSUE AND SERUM BIOCHEMICAL INDEXES OF MICE

To evaluate the acute lung toxicity and the effect on serum biochemical indexes of inhaled TiO2 nanotubes , healthy and adult Kunming mice are exposed to aerosols of TiO2nanotubes in a sealed chamber , the concentration of which is 250mg / m 3 while another group of mice are exposed to room air only served as control.The blood , alveolar lavaged fluid and lungs of the mice are collected and examined after exposed for 7 , 14and 28d , respectively.The serum analysis shows that glucose ( Glu ) values with 7dexposure , alanine aminotransferase ( ALT ) and aspartate aminotransferase ( AST ) activities with 28dinhalation , and total bile acid ( TBA ) values with 7 , 28d as well as the creatine kinase ( CK ) levels with 28dexposure are significantly different from those of controls ( P< 0.05 ) .The pathological findings exhibit that more TiO 2 nanotubes are found in the interstitium of pulmonary alveoli with the experimental time prolonged.The results suggest that TiO 2 nanotubes do produce adverse responses to the lung and serum biochemical indexes of mice.Moreover , the responses become severer with the exposed-time prolonged.     

Statistical study of electrostatic solitary waves associated with reconnection: Geotail observations

The role of waves in the dynamics of the magnetotail has long been a topic of interest in magnetospheric physics. The characteristics of Electrostatic Solitary Waves (ESWs) associated with reconnection have been studied statistically in the magnetotail by surveying the large amounts data obtained from Waveform Capture (WFC) which is an important component of Plasma Wave Instrument (PWI) on the Geotail spacecraft. About 150 reconnection events with WFC data available are selected, and approximately 10 thousands of ESW waveforms are picked up by hands for statistical study. The ESWs are observed near diffusion region and near the plasma sheet boundary layer (PSBL). Two kinds of waveforms of ESWs are observed: bi-polar and tri-polar pulses. It is found that the pulse width of the ESWs is in the order of 1–5 ms and the peak-to-peak amplitude is in the order of 0.1–5 mV/m. The amplitudes of ESWs are larger in the near-earth tail region than that in deep tail region. ESWs have been observed with or without guide magnetic field 〈By〉. The characteristics of ESWs in different reconnection region and under different strength of guild magnetic field, their possible generation mechanism will be discussed.