一种仿生附着装置柔顺关节的优化设计

为提高仿生附着装置在捕获空间非合作目标物时对目标运动参数的适应性,设计了一种3自由度串联柔顺关节,可通过关节嵌入系统后的协调运动来辅助装置被动适应运动目标物姿态,并在运动过程中基于弹簧、阻尼缓冲器组成的关节柔顺机构及其能量耗散原理来降低目标物动能。为验证、优化关节性能,通过ADAMS虚拟样机软件建立了基于柔顺关节的仿生附着装置捕获过程运动学与动力学模型,分析了柔顺关节3组弹簧刚度系数、黏滞阻尼系数对非合作目标物捕获状态的影响,并利用ADAMS-iSIGHT联合仿真平台,通过多岛遗传算法对上述弹簧、阻尼器的重要参数进行了优化,极大提高了柔顺关节的能量耗散效果,同时保证了可捕获目标物运动参数达到规定要求。      

序列图像中直线边缘快速提取和匹配

针时飞行器视觉导航等实时性较强的应用,给出了一种在航空序列图像中进行直线边缘快速提取和匹配的方案。在提取直线边缘时,运用了当前速度较快的邻接元素标记方法,从而提高了直线边缘提取速度。而在时直线边缘进行匹配时,给出了一种分三步走的方案,并提出了一种能够有效降低噪声影响的度量方式。首先选择3条直线边缘作为参考模型,在直线边缘的方向、位置以及物理特性的约束下构建候选匹配基,然后在基于矢量技术的基础上确定与参考模型基相对应的匹配模型,在此基础上再确定其他直线边缘之间的对应关系。试验结果表明,本文的直线边缘匹配方法比现有的方法速度提高了30倍以上,能够有效地满足一些实时性较强的应用。     

输送线网络监控系统的设计与实现

对可编程控制器控制原理进行分析,提出一种在已有设备的基础上进行改造,从而实现基于网络的监控技术。通过RS-485数据传输技术,运用TCP/IP协议,用MCGS(Mon itor and Control Generated System)组态软件编写程序软件,以图形界面实现对输送线的过程进行监控。     

空间非合作目标多指包络抓捕路径设计

针对现有空间非合作目标抓捕中存在无固定抓捕点以及待抓捕目标存在动态性等问题,提出了一种"主-从"式多指包络抓捕路径设计算法。首先,为了降低多指包络构型设计中的自由度,将多指机构分为一根主手指和其余从手指两类。然后,为了实现对具有动态性的空间非合作目标的抓捕,采用误差跟踪控制方法使主手指的基关节与包络点之间的运动保持同步。接着,引入单向距离的概念衡量主手指构型和包络边相似度,并利用快速搜索随机树算法寻找使得单向距离最小的主手指关节角取值。进一步,根据多指机构的结构模型,确定其余从手指的构型。最后,根据包络条件选择能够约束住空间非合作目标运动的有效包络构型。通过对可以简化为扁平型的空间非合作目标和一般性三维空间非合作目标这两类目标的包络抓捕仿真可以得出,所设计的算法可适用于一般性空间非合作目标的包络抓捕,同时计算复杂度也大大降低。     

Real-time GLE alert in the ANMODAP Center for December 13, 2006

Within the last years, a real-time system to monitor high energy cosmic rays for space weather use has been operated at Athens cosmic ray station. Neutron monitors and satellite high resolution data in real time are used, making it possible to observe cosmic rays in dual energy range observations. In large solar energetic particle (SEP) events, ground level enhancement (GLE) can provide the earliest alert for the onset of the SEP event. This system watches for count rate increases recorded in real time by 23 neutron monitors, which triggers an alarm if a ground level enhancement (GLE) of cosmic ray intensity is detected.     

The onset of sunspot cycle 24 and galactic cosmic ray modulation

The annual mean sunspot number (SSN) has a minimum value in 2008, while the monthly mean SSN has a value of zero in August 2009. The galactic cosmic ray modulation for cycle 24 began at earth orbit in January 2010. We study the onset characteristics of the new modulation cycle using data from the global network of neutron monitors. They respond to time variations in different segments of the galactic cosmic ray rigidity spectrum. The corresponding temporal variations in the interplanetary magnetic field intensity (B) and solar wind velocity (V) as well as the tilt angle of the heliospheric current sheet are also studied. There is a lag of 3 months between a large, sharp increase of the tilt angle of the heliospheric current sheet and the onset of modulation. Some neutron monitors are undergoing long-term drifts of unknown origin.     

三维RTPN的追踪导引研究

描述三维RTPN导引的模型是超越非线性微分方程组，不易求解．常规的方法是进行线性化。通过坐标系的变换和引入辅助向量获得了解析的捕获域和截获时间，并在三维空间内对这种追踪导引过程进行了仿真验算。理论分析和仿真表明：所设计的追踪导引律，能使整个追逃过程是在一个由初始相对距离和初始相对速度确定的平面内进行；当导弹采用RTPN导引，目标分别以IPN、RTPN逃逸和非机动飞行时，拦截TPN逃逸导引的目标能量消耗大，截获时间长，捕获域小。     

Tests for coalescing binary neutron stars as cosmological origin of gamma-ray bursts

Theoretical logN-logS distributions and (V/V _max) tests of gamma-ray bursts in the model of coalescence of neutron star (NS+NS) and/or NS+black hole (NS+BH) binaries are calculated for a flat Universe (=1) with different values of the cosmological constant and under various assumptions about the star formation history. The observed logN-logS distribution and value of (V/V _max)=0.33 for 411 bursts with knownC _max/C _lim from the 2d BATSE catalogue are best fitted with a model for which = 0.2 and primary star formation occurs at redshiftsz5–6.     

Hard X-ray emission from the recurrent transient A0535+26 during its 1980 high-intensity outburst

The transient X-ray pulsar A0535+26 was observed on October 4, 1980 during a high level intensity outburst with a balloon borne hard X-ray detector. High statistical quality source spectra were determined up to 100 keV. Both blackbody and Wien laws fit well the data. Pulse phase spectroscopy shows variation of temperature index between 7.5 and 8.5 keV in the off source spectra and between 7.4 and 10.5 keV in the off pulse spectra. The time averaged luminosity above 30 keV is 8×10³⁶ erg/s.