Polarizing gas at small optical depths around Algols

The origins of visible-band linear polarimetry of Algols and objects related to them are reviewed. It is pointed out, not for the first time, that the polarization signals of these systems can vary sporadically by significant amounts. The difficulty of evaluating the interstellar component of the observed polarization is discussed and these components are evaluated anew for each object studied in this paper. With one possible exception, the polarization signals intrinsic to these binaries derive from electron scattering. A well-defined model is applied to the constant and variable (but phase-locked) polarization signals. Limits to the mass associated with a scattering disk in each binary are derived. Within broad limits, concentrations of scattering mass within and above or below the orbital plane are also developed as are the centroid longitudes of these concentrations within the system. It is pointed out that very few measures of visible-band, circular polarization have been made but that cm-wavelength measures of Algol itself have been very informative.     

Comment on "Gyro Misalignment and Encoder Quantization Effects During Multi-Axis Evaluation of Strapdown Gyros"

A recent paper1 discusses certain aspects of strapdown attitude error sources. It is pointed out here that the long term effects of these and several additional sources have previously been determined, within the framework of a complete attitude reference [4] and navigation [5] system.     

Type-III radio bursts and their interpretation

The observations of type-III solar radio bursts are briefly reviewed to set requirements on a model for their interpretation. The most important of these requirements is that the source must be an electron stream which is in a state of continuous quasilinear relaxation and which initially must have a nearly monotonically decreasing velocity distribution. The problem of constructing a model is broken into three parts: (1) The plasma wave source which depends on the interaction of the electron stream with electron plasma waves. (2) The radiation source which depends on the interaction of plasma waves and transverse electromagnetic waves or in a magnetized plasma the ordinary and extraordinary modes of magnetoionic theory. (3) The propagation of radiation between the source and the observer which depends on the transmission of radiation through a scattering refracting absorbing magnetized plasma.Progress on a model for the plasma wave source is reviewed and it is concluded that no existing models are adequate. The equations which would lead to an adequate model are written down, but not solved. These include, in addition to collisional damping, Landau damping both by the exciting stream and the background plasma, and spontaneous and induced processes for a three-dimensional distribution of plasma waves. Possible limitations to a quasilinear approach such as pile-up of plasma waves and nonlinear effects are considered. Processes which affect the gross structure of the source such as electron trajectories in coronal streamers and electron scattering by inhomogeneities are reviewed.Progress on the radiation source is considered both in the absence and presence of a magnetic field. At high frequencies (e.g., 80 MHz) observations of radiation near the fundamental and second harmonic of the plasma frequency allow a unique determination of source size and the energy density in plasma waves within the uncertainties of geometry by source ray tracing. This determination is extremely critical because the fundamental must be amplified and thus production of the fundamental is effectively a much more highly nonlinear process than production of the second harmonic. At low frequencies (e.g., 500 kHz) the second harmonic is shown to be dominant because amplification of the fundamental becomes an inefficient process.Calculations of scattering of radiation in a random medium are reviewed. It is concluded that these are adequate at high and low frequencies, but have not been carried out properly at intermediate frequencies where amplification of the fundamental may still be present. It is shown in particular that when scattering is taken into account at high frequencies all observations can be explained by isotropic emission near the second harmonic. At low frequencies the nature of the scatterers is determined by source occultations unlike the case at high frequencies where these are free parameters. This fact allows the possibility of determining true source sizes at low frequencies by subtracting out the contribution due to scattering. A mechanism for producing the possibly observed linear or highly elliptical polarization of type-III bursts, which must be imposed far from the source due to Faraday rotation, is reviewed.Finally, the questions of what remains to be done and what we can hope to obtain upon completion of this work are briefly considered.The National Center for Atmospheric Research is sponsored by the National Science Foundation.     

航空发动机吸入颗粒物静电感应特性的模拟实验及分析

利用静电传感器和SC-010型环境试验箱等硬件搭建了吸入颗粒物静电监测模拟实验平台,并在此实验平台上展开了针对航空发动机吸入颗粒物静电感应特性的模拟实验研究,成功获取相应静电监测信号。实验设置颗粒材料、管道流速、颗粒粒径和颗粒投入质量4种变量作为变量条件,分别进行4组单一变量的对比实验,采集在不同颗粒材料、不同管道流速、不同颗粒粒径以及不同颗粒质量浓度环境下带电颗粒所产生的静电感应信号,对每组实验信号的活动率水平(AL)、正/负事件率(PER/NER)和绝对平均幅值等特征参数进行相应的数据分析和对比,并得到了一些有用的结论。实验发现,上述4种变量条件分别对静电感应信号的绝对时域平均幅值、AL参数、PER/NER参数有不同程度的影响。     

Radar target identification of aircraft using polarization-diversefeatures

The characteristics and target identification potential of a representation of the information from two polarization-diverse measurements of the radar backscatter of an unknown target are considered. The locus of these two polarization-diverse waveforms, termed the transient polarization response (TPR), has been shown to be closely related to the geometry of the scattering centers of the target. The polarization-related components of features derived from the TPR concur well with the shape and orientation of the major scattering centers distributed in the downrange profile of the object. This illustrates the intuitively appealing result that the polarization of the backscatter, as represented by the TPR and mapped onto the modified polarization chart, is determined by target geometry. It is shown that both polarization-related and amplitude-related features derived from the TPR are useful for target identification. By using distance measures that depend on various components, the elliptical parametrization information alone is sufficient to allow satisfactory target identification at SNRs of 0 dB and above. The significance of this result is that the absolute amplitudes of the received horizontally polarized and vertically polarized channels need not be known. However, if amplitude information is known, target identification percentages improve     

飞行器表面缝隙电磁散射特性研究

 在常规飞行器的各类电磁散射源中,缝隙属于弱散射源,但对于隐身飞行器,缝隙电磁散射不可忽略。为研究飞行器缝隙电磁散射特性,在不同极化下,将缝隙置于金属平板的对角线,削弱金属边缘电磁散射影响。通过系列雷达散射截面(RCS)测试分析,得到了缝隙电磁散射随缝隙宽度、（多缝隙）缝隙间距的变化规律,以及其极化特性。不同宽度单缝测试结果表明:对于水平极化,缝隙宽度小于波长的1/4时,缝隙的宽度增加将导致缝隙引起的表面波散射快速增长,反之,呈下降趋势;对于垂直极化,缝隙宽度较小时试件的电磁散射与无缝金属平板接近,当缝隙宽度大于波长的1/2时,宽度增加时,其散射增强。多缝隙测试结果表明缝隙间距会影响散射的空间分布、波峰位置,可以理解为对各单缝隙散射叠加效果的影响。垂直极化影响强于水平极化。     

DOA and polarization estimation via signal reconstruction with linear polarization-sensitive arrays

This paper addresses the problem of direction-of-arrival(DOA) and polarization estimation with polarization sensitive arrays(PSA), which has been a hot topic in the area of array signal processing during the past two or three decades. The sparse Bayesian learning(SBL) technique is introduced to exploit the sparsity of the incident signals in space to solve this problem and a new method is proposed by reconstructing the signals from the array outputs first and then exploiting the reconstructed signals to realize parameter estimation. Only 1-D searching and numerical calculations are contained in the proposed method, which makes the proposed method computationally much efficient. Based on a linear array consisting of identically structured sensors, the proposed method can be used with slight modifications in PSA with different polarization structures. It also performs well in the presence of coherent signals or signals with different degrees of polarization. Simulation results are given to demonstrate the parameter estimation precision of the proposed method.     

Resonant Scattering of X-ray Emission Lines in the Hot Intergalactic Medium

While very often a hot intergalactic medium (IGM) is optically thin to continuum radiation, the optical depth in resonant lines can be of order unity or larger. Resonant scattering in the brightest X-ray emission lines can cause distortions in the surface brightness distribution, spurious variations in the abundance of heavy elements, changes in line spectral shapes and even polarization of line emission. The magnitude of these effects not only depends on the density, temperature and ionization state of the gas, but is also sensitive to the characteristics of the gas velocity field. This opens a possibility to use resonant scattering as a convenient and powerful tool to study IGM properties. We discuss the application of these effects to galaxy clusters.     

On Processing Optical Images Propagated Through the Atmosphere

The problem of how to process optical images that have propagated through a turbulent atmosphere is considered. It is assumed that either the object or its (free-space) scattered field at the receiving aperture is known, except for unknown parameters that are to be estimated. Isotropic and homogeneous turbulence as discussed by Tatarski and Chernov is assumed. It is assumed that a very short (in time) reception is made, that the turbulence-induced complex phase errors are either small or have a correlation distance short relative to the receiving aperture extent, and that the object is within an isoplanatic region. The method of maximum likelihood (ML) is used as a criterion; its applicability is discussed. The ML image-processing structure is found and is nonlinear. Asymptotic cases are examined; among other conclusions, it is shown that the ML processing of independent receptions is more complex than an ML processing of the sum of the receptions. A coherent optical system that realizes the ML image processor is described; it includes the capability to generate the scattered field. Simplifications are pointed out.     

采用SBR法研究飞机进气道的雷达散射截面

采用弹跳射线法(SBR)对飞机发动机进气道的雷达散射截面(RCS)进行了分析计算.通过光学射线跟踪、场强跟踪及口径积分方法,研究了任意截面和形状的管道电磁散射特性,通过在微波暗室的实际测量,频率在X波段,分别进行垂直极化和水平极化两种方式测试,比较了一实际进气道的计算与实验结果,验证了此方法的有效性,与其他方法相比较,具有物理概念清晰、数学模型容易建立等特点,满足了实际应用的需要.     

螺钉/铆钉目标电磁散射特性的试验研究

通过系列化雷达散射截面（RCS）测试,研究了单列、多列螺钉/铆钉板在单站多方位、双站的散射特性,分析了不同极化方式、不同排列、不同方位角以及不同双站角对螺钉/铆钉散射的影响及关系。试验结果表明,圆头钉板水平极化明显强于垂直极化;沉头钉板水平极化仅略强于垂直极化。列距不同,由于相位叠加的不同,会导致叠加波峰的位置发生偏移,在设计时可平行间距布置,将散射方向集中。对双站散射,较小双站角时曲线与单站时有一定相似性,但波峰幅度和位置均发生较大变化;较大双站角时,电磁散射表现出耦合效应;双站角使测试曲线偏转,幅度为双站角的1/2;RCS均值随双站角增大而减小。     

台阶目标电磁散射特性研究

 通过系列雷达散射截面（RCS）测试,研究了单台阶板随台阶高度变化的规律,分析了多台阶板电磁散射与其高度、间距、极化方式之间的变化关系,并将台阶板散射结果与金属平板结果进行比较,定量总结了各参数对台阶板散射的影响。试验结果表明,台阶高度增加导致散射增强;多台阶间距增大引起曲线振荡增强,说明台阶间耦合作用加强,但RCS均值相对于平板均值增幅不变;多台阶散射表现为各台阶在不同相位上相互叠加的结果。     

基于计算电磁学方法的旋翼雷达散射截面特性

以Maxwell方程组为主控方程,时间离散采用4步Runge-Kutta法,空间离散使用MUSCL(monotonic upstream-centered scheme for conversation laws)格式与Steger-Warming通量分裂结合的方法,建立了一套基于时域有限体积法的旋翼RCS(雷达散射截面)特性数值计算方法.采用代数方法生成围绕旋翼的O型贴体、正交网格.在验证方法有效性基础上,着重分析了旋翼平面和翼型RCS极化、入射角、电尺寸等影响特性,并给出了翼型几何特点对RCS的影响规律;然后运用线性加权和法进行了旋翼翼型隐身性能的综合筛选.研究表明:旋翼RCS动态包络线是一个强散射水平的连续振荡区域;选取3片桨叶旋翼的最大雷达探测距离为2片桨叶的82.2%,且有利于控制旋翼的散射最大峰值.同时,HH02旋翼翼型在4个重要的散射角域,最大探测距离分别为NACA0012翼型的105.1%,99.4%,86.6%和83.5%,表明综合雷达隐身性能最好.     

Multipath Effects on an Azimuthal Monopulse System

The first topic considered is an analysis of the conditions under which the conventional definition of length of the glistening surface, as given by Beckmann and Spizzichino, is not valid. For some conditions, significant amounts of incoherent scattered power can be received from areas beyond the conventional length. A second topic is the investigation of the effect on azimuthal angular tracking accuracy due to such scattering factors as shadowing, surface height distribution, standard deviation in surface height ?, surface correlation length T, unevenness and inhomogeneity of the terrain, antenna heights, and signal polarization. A number of interesting results have been observed. The amount of additional incoherent power not included under the conventional definition depends on the ratio ?/T, except for the case where both transmitter and receiver are very close to the surface. The trends in the behavior of the glistening surface are similar for vertical or horizontal polarization, for Gaussian or exponential surface height distributions, and for different signal frequencies in the S-band to L-band range.     

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.     

A Recursive Method for Signal Resolution

A recursive method is given for resolving signals overlapping in time. Assume that the signal waveform is known and several signals are received. The signals (of unknown number) may overlap with one another and the amount of time delay of each individual signal is unknown. The signals are corrupted with additive white Gaussian noise. The problem is to estimate the number, the amplitudes, and the time delays of the overlapping signals. Assume that at a certain instant tk-1 estimates have been made on the number of signals arriving in the time interval (O, tk-1) and the amplitudes and time delays of these signals. Using these estimates, we test at tk the hypothesis H1 that a new signal arrives at tk against the null hypothesis Ho that no new signal arrives. The decision gives the number of signals arriving in the time interval (0, tk); the parameters are then re-estimated. The overlapping signals are detected and resolved, and the estimates are improved at each stage. The system is analyzed in detail, and computer-simulated results are presented.     

灵巧噪声干扰本质含义探讨

文章对灵巧噪声干扰概念的表述提出了质疑,在多项质疑中选取了SLB技术进行简要分析,并指出,SLC等抗干扰技术的作用与是否实施灵巧噪声干扰没有直接关系。进一步,基于匹配滤波器理论对灵工j噪声干扰的本质含义进行了分析,指出：灵巧噪声干扰的本质含义是使干扰由多个分量组成,并且使干扰中的每一个分量的频谱都与雷达发射信号的频谱相...     

Imaging of a compact range using autoregressive spectral estimation[radiation patterns measurement]

The spurious scattering mechanisms of a compact range, which cause spurious signals as well as the desired plane wave to illuminate the test zone, are addressed. It is shown that an accurate estimation of the direction-of-arrival and amplitude of spurious signals in a compact range is beyond the resolution available from the Fourier transform. An estimation technique based on autoregressive (AR) modeling of field probe data is developed to locate and quantify the spurious signal sources. The probe aperture is divided into a number of overlapping subapertures so that the far-field criterion for each subaperture is satisfied. Then, the subaperture data are modeled as an AR process. Singular value decomposition and forward-backward linear prediction are used to estimate the model order and the AR parameters. Examples of probe measurements and analysis for an actual compact range are given     

盲源分离及盲信号提取的研究进展

盲源分离和盲信号提取是从观测信号中恢复源信号的有效方法,目前已成为信号处理领域的研究热点。介绍了盲信号处理的数学模型,给出盲源分离与盲信号提取的基本思想,阐述了各方法的原理、特点及性能,并对它们之间的区别与联系进行分析,最后指出盲源分离及盲信号提取的发展方向。     

航空发动机砂尘吸入物静电监测仿真实验

提出了航空发动机砂尘吸入物静电监测的仿真实验方法,实验以软件ANSYS电磁场分析模块建立有限元模型为基础,模拟不同粒径、荷质比、运动速度及质量浓度情况下砂尘吸入物的静电感应信号,并分别从时域与频域对感应电荷与电压信号进行分析,研究砂尘吸入物的粒径及其他宏观参数与静电监测信号之间的关系,建立用以表征砂尘颗粒粒径大小的特征指标。基于IDMS(进气监测系统)感应电压信号功率谱密度分布建立了特征向量,并以其曼哈顿距离与欧氏距离作为特征指标表征砂尘颗粒粒径大小。经仿真实验验证:特征指标与砂尘粒径呈正相关,且不受砂尘吸入物运动速度及荷质比变化的影响,但受砂尘吸入物质量浓度影响。进一步研究将利用质量浓度对特征指标进行修正,并开展验证实验。