Fluctuating magnetic fields in the magnetosphere

The study of Extremely-Low-Frequency (ELF) and Very-Low-Frequency (VLF) waves in space has been intensively pursued in the past decade. Search coil magnetometers, magnetic loop antennas, and electric dipole antennas have been carried on board many spacecraft. The measurements performed by these instruments have revealed a multitude of wave phenomena, whose study in turn is providing a wealth of information on the physics of the magnetospheric and ionospheric plasma. Two classes of wave phenomena are observed: whistlers and emissions. The observed whistler phenomena include: multiple hop ducted whistlers, ion-cutoff whistlers, ion cyclotron whistlers, subprotonospheric whistlers, magnetospherically reflected whistlers and walking trace whistlers.The emissions observed at high altitudes near the magnetic equator differ in many respects from those observed at low altitudes near the ionosphere. At high altitudes, inside the plasmasphere ELF hiss is the dominant emission and outside the plasmasphere chorus is the dominant emission. Also seen is a sub-LHR hiss band in the outer plasmasphere near the equator, and high pass noise and broadband noise in the outer nightside magnetosphere. At low altitude both ELF hiss and chorus are present but, here, ELF hiss is the dominant emission even outside the plasmasphere. Additional emissions, specific to low altitudes, such as VLF hiss and LHR noise are also observed. Although the observations of these phenomena by spacecraft have been complemented by many ground-based and rocket borne studies as well as by spacecraft observations of man-made signals, this paper reviews only satellite observations of signals of natural origin.     

VLF waves: Conjugated ground-satellite relationships

The French mobile station for recording geophysical data has been put in operation at Husafell, Iceland (64°5N, 20°8W) between the 10th of July and the 22nd of September, 1977. This place was more or less conjugated with GEOS when this satellite was near its apogee. The equipments installed in the station for recording VLF and ULF phenomena have characteristics (band-pass, sampling rates) which are identical to the similar equipments installed onboard GEOS. Intercomparison between signals recorded at both points are therefore easy. We present here the results which were obtained in the VLF range.In many occasions, VLF emissions (mainly hiss) do present identical variations in amplitude, with a very abrupt (<1 mn) and very large (>20 dB) decrease in amplitude. Because of their simultaneity at both points, such abrupt variations cannot be interpreted in terms of a sudden ionospheric absorption (associated with an enhanced particle precipitation) nor in terms of a sudden crossing of detached plasma regions. In some cases, these abrupt changes in the VLF intensity are associated with the appearance and disappearance of strong ULF emissions, in the Pc-1 frequency range. Some examples of associated onboard measurements of high energy electron fluxes or cold plasma density (when available) are given, which may help understanding these VLF conjugated relationships.     

Interference Immunity Effects in CPSK Systems with Hard-Limiting Transponders

Transmission characteristics are described for M-ary coherent phase-shift keyed (CPSK) systems with N-stage hard-limiting transponders where noise and multiple continuous wave (CW) interference sources are additively combined in each link. A general expression for the probability density function of the composite phase at the final link is derived; the overall error probability is then obtained from this general expression. Comparisons with N-cascaded linear amplifier systems clearly show the noise and interference immunity that result from the use of bandpass hard limiters (BPHLs). The BPHL system's error probability improvement versus interference sources is shown to be much larger than the improvement versus noise.     

DEMETER Observations of EM Emissions Related to Thunderstorms

The paper is related to specific emissions at frequency <3 MHz observed by the low altitude satellite DEMETER in relation with the thunderstorm activity. At its altitude (～700 km), the phenomena observed on the E-field and B-field spectrograms recorded by the satellite are mainly dominated by whistlers. Particular observations performed by DEMETER are reported. It concerns multiple hop whistlers and interaction between whistlers and lower hybrid noise. Two new phenomena discovered by the satellite are discussed. First, V-shaped emissions up to 20 kHz are observed at mid-latitude during night time. They are centered at the locations of intense thunderstorm activity. By comparison with VLF saucers previously observed by other satellites in the auroral zones it is hypothesized that the source region is located below the satellite and that the triggering mechanism is due to energetic electrons accelerated during sprite events. Second, emissions at frequency ～2 MHz are observed at the time of intense whistlers. These emissions are produced in the lower ionosphere in probable relation with Transient Luminous Events (TLEs).     

Non-linear resonant excitation of whistler mode waves in the Earth's ionosphere

We examine the resonant non-linear interaction in the Earth's ionosphere of two powerful high frequency radio beams with frequencies f ₁ and f ₂ (both larger than the plasma frequency at F2_max) and wave numbers k ₁ and k ₂ such that a whistler mode wave can be excited with a frequency f ₃ = f ₁ — f ₂ and a wave number k ₃ = k ₁ – k ₂. The feasibility of an effective ground based installation, sited at low latitudes, is discussed and the field strength of the wave emerging from a 10 km wide ionospheric region illuminated by the beams is evaluated for a range of transmitted frequencies, beam orientations and plasma frequencies in the interaction region. It is suggested that the longitude dependence of the enhancement of VLF noise bands detected by the Ariel 3 satellite may be due to a non-linear interaction of this type between any two or more medium wavelength signals from areas where there is a high concentration of commercial broadcasting stations, such as the NE region of the U.S.A.     

飞机噪声技术研究——工程解决方法

 飞机噪声存在的3个问题：①机舱的噪声振动控制;②机场的噪声干扰;③某些部位的抗声疲劳设计。针对以上问题,综述了北京强度环境研究所进行过的飞行器噪声课题的研究工作,提出了大型飞机噪声问题的工程解决方法,包括：噪声载荷谱的确定;喷气噪声和客机机舱的噪声振动控制;声疲劳设计。研究了超声速喷流的相似准则,用热流缩比模型试验测定火箭的发射噪声载荷达到同样精度;对于飞机来说,实测比风洞测量更方便、更经济,实测气动噪声主要的困难是如何测量到真实的气动噪声,传声器的安装方法、飞行器表面的静压变化等;喷流噪声控制方法是冷空气缩比模型试验,介绍了冷空气缩比模型试验的原理和方法;论述了在结构的疲劳强度试验中必须采用统计分析方法的原理。从多方面论述了大型飞机噪声课题的研究,对于飞机的安全性、经济性、舒适性都是很重要的课题,对于发展中国大型飞机工程有很重要的现实意义。     

一种有效的消波装置

对无限长渠道中小振幅入射波通过两块间距为ｌ,透水性能不同的多孔透水板的反射和透射进行了研究。应用分离变量法得到了反射波和透射波的波形。结果表明,当ｌ为入射波半波长的倍数时,反射波和透射波振幅最大,消波效果差,最佳消波率为５０％。当ｌ为入射波１／４波长加半波长的倍数时,反射波和透射波振幅最小,消波效果好,最佳消波率大于５０％。此外,还得到了无反射波的条件。     

Observations of ion cyclotron waves near synchronous orbit and on the ground

Ion cyclotron waves (hereafter ICW's) generated in the magnetosphere by the ion cyclotron instability of 10–100 keV protons are now known to be the origin of short-period (0.1–5 Hz) electromagnetic field oscillations observed by synchronous spacecraft and on the earth's surface. Observations of the various wave characteristics, including spectral and polarization properties that lead to the identification of generation and propagation mechanisms and regions in the magnetosphere are described with reference to ATS-6, GEOS and ground-based wave data and interpreted using cold plasma propagation theory. The presence of heavy ions (O⁺, He⁺) dramatically modifies ICW magnetospheric propagation characteristics giving rise to spectral slots and polarization reversals. These properties may be used in plasma diagnostics. Finally satellite-ground correlations and techniques for determining the magnetospheric source position of ICW's not seen at synchronous orbit but observed on the ground as structured Pc1 pulsations are considered.     

Waves in space plasmas: Highlights of a Conference held in Hawaii, 7–11 February 1983

The Conference was called to bring together investigators of magnetospheric plasma waves having frequencies from VLF whistlers and emissions down through ELF and ULF to Pc5 long period pulsations. The emphasis was on the physics and techniques underlying the entire frequency range. Topics included wave electron interactions and electron precipitation, ray tracing and other methods to track down sources of VLF and ULF waves, VLF-ULF relationships, heavy ion effects in ULF propagation, and long period ULF waves.     

Fluctuating magnetic fields in the magnetosphere

The study of ULF waves in space has been in progress for about 12 years. However, because of numerous observational difficulties the properties of the waves in this frequency band (10^-3 to 1 Hz) are poorly known. These difficulties include the nature of satellite orbits, telemetry limitations on magnetometer frequency response and compromises between dynamic range and resolution. Despite the paucity of information, there is increasing recognition of the importance of these measurements in magnetospheric processes. A number of recent theoretical papers point out the roles such waves play in the dynamic behavior of radiation belt particles.At the present time the existing satellite observations of ULF waves suggest that the level of geomagnetic activity controls the types of waves which occur within the magnetosphere. Consequently, we consider separately quiet times, times of magnetospheric substorms and times of magnetic storms. Within each of these categories there are distinctly different wave modes distinguished by their polarization: either transverse or parallel to the ambient field. In addition, these wave phenomena occur in distinct frequency bands. In terms of the standard nomenclature of ground micropulsation studies ULF wave types observed in the magnetosphere include quiet time transverse — Pc 1, Pc 3, Pc 4, Pc 5 quiet time compressional — Pc 1 and Pi 1; substorm compressional Pi 1 and Pi 2; storm transverse — Pc 1; storm compressional Pc 4, 5. The satellite observations are not yet sufficient to determine whether the various bands identified in the ground data are equally appropriate in space.Publication No. 982. Institute of Geophysics and Planetary Physics, University of California, Los Angeles, Calif. 90024.     

基于模态波理论的压气机失速先兆识别方法

针对压气机气动失速预警存在无法兼顾对渐进型和突尖型失速先兆有效识别的不足，以及提取失速团幅值需要多路传感器信号的局限。分析了压气机失速发展过程中的信号特征；根据压气机失速信号的旋转特性，提出基于单路传感器信号重构周向多路失速先兆信号的方法，讨论了信号重构步长的取值；基于模态波理论，通过对重构信号进行空间傅里叶变换，得到失速扰动信号各阶模态幅值，根据低阶模态的幅值变化实现对渐进型与突尖型失速先兆的识别。以某压气机为例进行仿真，结果表明:当信号重构的步长小于突尖波时间尺度的一半时，重构的多路信号能够复现压气机周向位置失速发展过程，且步长越小，越有利于失速先兆的识别；由模态分解得到的1阶模态幅值的变化能够有效反映失速发展过程；通过合理设置模态幅值的阀值，可以在失速发展前期对失速先兆进行准确识别，从而，基于单路传感器失速信号即可实现对渐进型失速和突尖型失速均能进行预警。      

Signal Interference and Improvement of Signal-to-Noise Ratios in a Half-Wave Linear Detector

Signal interference in the half-wave linear detector has been studied only for amplitude modulation. In this paper, we treat signal interference for both an amplitude-and an angle-modulation communication system. The input to the half-wave linear detector is assumed to be composed of an amplitude-modulated wave, an angle-modulated wave, and narrow-band Gaussian noise. In particular, when strongweak relations exist in the input processes, a detailed analysis for the output component is presented to clarify some useful output properties.     

Interplanetary shock waves generated by solar flares

Recent observational and theoretical studies of interplanetary shock waves associated with solar flares are reviewed. An attempt is made to outline the framework for the genesis, life and demise of these shocks. Thus, suggestions are made regarding their birth within the flare generation process, MHD wave propagation through the chromosphere and inner corona, and maturity to fully-developed coronal shock waves. Their subsequent propagation into the ambient interplanetary medium and disturbing effects within the solar wind are discussed within the context of theoretical and phenomenological models. The latter — based essentially on observations — are useful for a limited interpretation of shock geometric and kinematic characteristics. The former — upon which ultimate physical understanding depends — are used for clarification and classification of the shocks and their consequences within the solar wind. Classification of limiting cases of blast-produced shocks (as in an explosion) or longer lasting ejecta (or piston-driven shocks) will hopefully be combined with the study of the flare process itself.The theoretical approach, in spite of its contribution to clarification of various concepts, contains some fundamental limitations and requires further study. Numerical simulations, for example, depend upon a non-unique set of multi-parameter initial conditions at or near the Sun. Additionally, the subtle but important influence of magnetic fields upon energy transport processes within the solar wind has not been considered in the numerical simulation approach. Similarity solutions are limited to geometrical symmetries and have not exploited their potential beyond the special cases of the blast and the constant-velocity, piston-driven shock waves. These continuum fluid studies will probably require augmentation or even replacement by plasma kinetic theory in special situations when observations indicate the presence of anomalous transport processes. Presently, for example, efforts are directed toward identification of detailed shock structures (as in the case of Earth's bow shock) and of the disturbed solar wind (such as the piston).Further progress is expected with extensive in situ and remote monitoring of the solar wind over a wide range of heliographic radii, longitudes and latitudes.This paper is a revised and updated version of an invited review originally presented at the IUGG XV General Assembly, Moscow, U.S.S.R., 2–14 August 1971.     

Hydrodynamic shock wave formation in the solar chromosphere and corona during flares

Basic mechanisms of the hydrodynamic shock wave formation in the solar atmosphere during flares are considered. Hydrodynamic plasma flows during flares arise due to fast energy release which is accumulated in the magnetic field of currents in the solar atmosphere. Shock waves arise as a result of rapid heating of the chromospheric upper layers from accelerated particles or heat fluxes. Powerful hydrodynamic phenomena can also arise due to explosive current sheet disruption in the region of strong magnetic field reconnection. Fundamental questions of shock wave formation and propagation in a non-homogeneous emitting solar atmosphere are discussed.An invited paper presented at STIP Workshop on Shock Waves in the Solar Corona and Interplanetary Space, 15–19 June, 1980, Smolenice, Czechoslovakia.     

Type Pi 1–2 magnetic field pulsations

The relationships of type Pi (broadband) pulsations to various other substorm-related phenomena are reviewed. Several of the more popular mechanisms for the origin of Pi activity are discussed in the light of the observations. There is only one mechanism in sight that tentatively accounts for observed characteristics of Pi 1–2 activity at auroral oval and polar cap latitudes and that is the three-dimensional current loop mechanism. If two or more mechanisms are involved in the generation of Pi noise, then it is possible that the garden-hose overstability and/or a drift Alfvén wave mechanism operating in the plasma sheet contribute to the observed pulsations.The common feature of all Pi 1–2 events is not the presence of temporal precipitation pulsations but the presence of an E-region, suggesting that enhanced conductivity and E-region currents are required. Pi activity appears to be closely related to unsteady convection in progress. Pi data promise to provide useful information on convection and field-aligned and ionospheric currents.     

Stimulation of VLF amplification in the magnetosphere

Among the various plasma instabilities that exert influence on the dynamic equilibrium state of the magnetosphere, the cyclotron-resonance interaction appears to be the most accessible to artificial stimulation. The strength of the interaction is sensitive to both the background magnetoplasma parameters and the hot energetic particle distribution. Thus, proper modification of one or more conditions can induce significant wave amplification at the expense of hot plasma energy density. Several methods of hot and cold plasma injection have been investigated with the linear theory to assess their effectiveness as a means of stimulating amplification.Only the interaction of VLF waves (3–30 kHz) with hot electrons (0.1–100 keV) is treated here. The injection of a dense jet of barium that travels upward along the geomagnetic field causes appreciable amplification when the jet is within 30° of the geomagnetic equator. Injection of a geosynchronous lithium cloud stimulates amplification of both VLF and ULF waves, but the magnitude depends critically on the state of geomagnetic activity. Conventional hot electron beams may also amplify narrow frequency bands, but the net wave energy is severely limited by the beam energy.Although the cyclotron-resonance is recognized as a dominant interaction in magnetospheric dynamics, its properties have never been confirmed quantitatively by appropriate spacecraft experiments. Controlled injections would provide important insight into this fundamental process because the induced amplification has a well-defined signature.     

航空声学风洞3/4开口试验平台地板对远场噪声测量的影响

利用Kirchhoff-Helmholtz声学理论建立了地板声波反射问题的时域理论模型,推导了地板面上反射波的幅值函数和延迟时间的表达式,并引入了恰当的数值方法对反射声场进行求解,理论方法的正确性得到了实验结果的验证。以典型的高斯调制正弦波脉冲和连续正弦波为例,用建立的理论方法对噪声信号的传播过程和平台地板对远场噪声测量的影响进行了数值模拟研究,结果表明：地板的存在将使得远场接收到的噪声信号中出现直达波和反射波,反射波包含了中心波和边缘波。在低频段,地板宽度增加,远场噪声声压级增大;在高频段,地板宽度增加对远场总噪声级影响不明显。对于高速列车（HST）模型,车底位置的声源比车顶位置的声源在高频段受到地板反射的影响更大。     

航空发动机气路故障诊断的SANNWA-PF算法

针对航空发动机非线性、非高斯的特点，提出一种用于航空发动机气路故障诊断的自适应神经网络权值调整粒子滤波（SANNWA PF）算法。该算法根据粒子分布情况确定分裂和调整的粒子数目，进而根据粒子权重采用正态分布的方式进行分裂，采用反向传插(BP)神经网络进行权值调整，缓解了粒子的退化和贫化，具有更强的自适应性能和跟踪能力。通过一维非线性跟踪模型和航空发动机气路故障诊断仿真研究表明:SANNWA PF算法具有良好的非高斯性能，相对粒子滤波一维非线性追踪模型估计精度提高约21%，航空发动机气路故障诊断在高斯噪声和非高斯噪声下分别提高约30%和26%，诊断速度分别提高约7倍和10倍。      

比例与非比例加载下30CrMnSiA钢多轴高周疲劳失效分析

为了分析比例与非比例加载下,30CrMnSiA钢的多轴高周疲劳的失效规律。通过对30CrMnSiA钢材料开展比例与非比例(δ=90°)加载下的多轴高周疲劳试验,研究了应力幅比和相位差对疲劳寿命、断口特征及裂纹起裂角度的影响。试验结果表明,对于比例与非比例加载,随着应力幅比的增大,多轴疲劳寿命逐渐增加。对疲劳断口分析发现,裂纹萌生于试件表面,断口有明显的疲劳源区、扩展区和瞬断区,不同加载路径下的试件断口形式有明显差异。通过对起裂角度的分析发现,应力幅比大于0.25时表面裂纹有明显的第Ⅰ阶段向第Ⅱ阶段的转变,且第Ⅰ阶段沿着接近最大剪应力幅值平面方向扩展,第Ⅱ阶段沿着接近最大正应力平面方向扩展。此外,对典型试件的疲劳断口及表面扩展路径进行了分析,研究表明多轴疲劳试验试件裂纹的特征比值在0.3~0.5之间,且裂纹沿深度方向扩展至300 μm时占总寿命的85%以上。      

一种射频噪声干扰信号品质因素改进方法

针对射频噪声干扰信号直接限幅引起的干扰信号品质降低问题,分析了射频噪声干扰直接限幅造成的影响,在射频噪声干扰信号品质因素理论模型基础上,提出 1种基于双地址序列读取的射频噪声干扰信号品质优化方法。通过设置双地址寻址方式,改进基带噪声数据读取方式,提高限幅条件下的射频噪声干扰信号品质因素。仿真实验表明,该优化方法能够在直接限幅条件下提高干扰信号的品质因素,并基于 FPGA进行了硬件测试,验证了该方法的可行性。