数字示波器在尖峰干扰脉冲强度测量中的应用

运用数字示波器瞬态捕获能力及面积测量功能，快速、准确、不遗漏地测量电子设备的尖峰干扰信号（脉冲信号），用公式将脉冲强度单位换算为脉冲频谱密度单位。     

Multifractal Spectrum and Calculation

多重分形理论是进行信号奇异性处理的有用工具 ,由于只有少数集合的多重分形谱可以有解析表达式 ,多重分形谱的计算是其中重要而又较难处理的问题 .简要介绍了多重分形理论的一种形式体系 ,提出了一种采用动态链表来进行多重分形谱计算的方法 ,大幅度地降低了对存储器容量的要求 .用所提出的方法对康托集进行了计算 ,计算结果与理论结果相符 ,表明了算法的有效性 .     

计算大型实对称特征问题的 Lanczos-QR 算法

为了计算大型实对称特征值问题Ｋｘ＝λＭｘ的少数低阶特征值对，本文给出Ｌａｎｃｚｏｓ－ＱＲ迭代方法。首先，给定初始迭代向量ｖ１，作ｍ步Ｌａｎｃｚｏｓ分解：ＫＶｍ＝ＭＶｍＴｍ＋ｈｍｅｍＴ。取Ｔｍ的ｄ个最大特征值为移位量，对Ｔｍ进行ｄ步带原点位移的ＱＲ分解。然后，修改初始迭代向量ｖ１。迭代地重新开始这一过程，迫使初始迭代向量ｖ１进入需求的特征子空间，从而使残量‖Ｋｘ－θＭｘ‖→０。数值例子表明，该方法收敛性强，且稳定、有效。     

On the electrodynamics of counter stream in pulsar’s inner annular cap region

The electric properties of pulsar’s inner annular gap are explored in this paper. Under two main assumptions, (1) the pulsar is alive, (2) the total charge of pulsar should not vary with time, the condition for the acceleration of negative particle in the annular region is derived. The acceleration condition is j₋ ? 0.5j₊, i.e., the current carried by negative particles is greater than or equal to 0.5 times of the current carried by positive particles. This condition holds even when the backward flow of positive particles exists in the annular region. It is noted that the outflow of negative particles offers good opportunities to understand the current closure problem of pulsar as well as wide radiation beam of pulsar observed at high energy band.     

疲劳开裂结构等效分析谱构造方法

为了解决外场疲劳裂纹排故中结构疲劳载荷谱数据不全或过于复杂的问题,提出了一种适用于飞机外场疲劳开裂结构的等效分析谱构造方法。该方法以细节疲劳额定值(DFR)法和结构细节有限元分析为基础,构建地—空—地最大应力与结构疲劳寿命的变化曲线,进而通过寿命反推,获取适用的地—空—地损伤比,以此构建等效分析谱,谱型为等幅谱。通过应用实例,将该方法构造的载荷谱与实测谱进行了对比,确认了该方法的正确性和有效性。     

铝合金含硅量的测定方法

Ｎ２Ｏ－Ｃ２Ｈ２原子吸收光谱法测定卫星系统电池外壳铝合金中的硅含量。讨论了燃烧器高度、燃助比、共振线等测定条件的选择方法，以及酸度、温度和Ｎ２Ｏ－Ｃ２Ｈ２火焰区对测定精度的影响。实际应用证明，该方法灵敏度高，干扰小，选择性和重复性好，并具有操作简便，易掌握，分析周期短等特点；精密度和准确度均能满足卫星系统电池外壳体研制的要求。     

频谱分析法在静止气象卫星调焦分析中应用研究

利用频谱分析方法，对静止气象卫星扫描辐射计的在轨调焦进行快速、准确的分析判断，确定是否需要调整及调整时所发遥控命令的调整方向和步长等，避免了单向调出焦距极限位置时，对辐射计造成永久性损坏。文章首次提出的二维频谱法，即使在图像定位精度不高的情况下仍然适用，可以得出准确的分析结果。     

卫星遥测功率谱分析和调制度测量方法研究

残余载波调制是卫星测控中的常用调制体制。文章从理论上给出了该体制下信号的功率谱密度表达式，得到奇次谐波谱线展宽等结论，并通过仿真和实验进行了验证。利用所得结论讨论了遥测调制度测量方法，提出通过功率谱的2阶边带进行测量可以使结果得到改善。     

圆球绕流场的尾涡分析和升阻力研究

采用自编的分块算法程序模拟了雷诺数在20～1000之间的圆球绕流场.在Re=25时捕捉到流动分离,与试验结果一致.对Re=250时稳态非对称尾流区内流体的输运情况进行研究,证实圆球绕流场中纵向对称面的存在.对于非稳态流动,主要研究了阻力和横向力的时间变化规律,并分析了频谱特征.计算发现横向合力主要在横截面上两个很窄的区间内偏移.经过几种不同涡定义方法的优劣测试,本文采用Hunt等人介绍的Q-定义方法对非稳态绕流场的尾涡结构进行了直观描述.     

Particle Acceleration Mechanisms

In this paper we review the possible mechanisms for production of non-thermal electrons which are responsible for the observed non-thermal radiation in clusters of galaxies. Our primary focus is on non-thermal Bremsstrahlung and inverse Compton scattering, that produce hard X-ray emission. We first give a brief review of acceleration mechanisms and point out that in most astrophysical situations, and in particular for the intracluster medium, shocks, turbulence and plasma waves play a crucial role. We also outline how the effects of the turbulence can be accounted for. Using a generic model for turbulence and acceleration, we then consider two scenarios for production of non-thermal radiation. The first is motivated by the possibility that hard X-ray emission is due to non-thermal Bremsstrahlung by nonrelativistic particles and attempts to produce non-thermal tails by accelerating the electrons from the background plasma with an initial Maxwellian distribution. For acceleration rates smaller than the Coulomb energy loss rate, the effect of energising the plasma is to primarily heat the plasma with little sign of a distinct non-thermal tail. Such tails are discernible only for acceleration rates comparable or larger than the Coulomb loss rate. However, these tails are accompanied by significant heating and they are present for a short time of <10⁶ years, which is also the time that the tail will be thermalised. A longer period of acceleration at such rates will result in a runaway situation with most particles being accelerated to very high energies. These more exact treatments confirm the difficulty with this model, first pointed out by Petrosian (Astrophys. J. 557:560, 2001). Such non-thermal tails, even if possible, can only explain the hard X-ray but not the radio emission which needs GeV or higher energy electrons. For these and for production of hard X-rays by the inverse Compton model, we need the second scenario where there is injection and subsequent acceleration of relativistic electrons. It is shown that a steady state situation, for example arising from secondary electrons produced from cosmic ray proton scattering by background protons, will most likely lead to flatter than required electron spectra or it requires a short escape time of the electrons from the cluster. An episodic injection of relativistic electrons, presumably from galaxies or AGN, and/or episodic generation of turbulence and shocks by mergers can result in an electron spectrum consistent with observations but for only a short period of less than one billion years.