Modified fast Fourier transform in FBMC for satellite communications

In this paper,a Doppler scaling fast Fourier transform (Doppler-FFT) algorithm for filter bank multi-carrier (FBMC) is proposed,which can efficiently eliminate the impact of the Doppler scaling in satellite communications.By introducing a Doppler scaling factor into the butterfly structure of the fast Fourier transform (FFT) algorithm,the proposed algorithm eliminates the differences between the Doppler shifts of the received subcarriers,and maintains the same order of computational complexity compared to that of the traditional FFT.In the process of using the new method,the Doppler scaling should be estimated by calculating the orbital data in advance.Thus,the inter-symbol interference (ISI) and the inter-carrier interference (ICI) can be completely eliminated,and the signal to interference and noise ratio (SINR) will not be affected.Simulation results also show that the proposed algorithm can achieve a 0.4 dB performance gain compared to the frequency domain equalization (FDE) algorithm in satellite communications.     

Intersymbol and CW Interference in QPSK, OQPSK, and MSK Hard-Limiting Satellite Systems

A new equivalent model for deriving the bit error rate (BER) of quadrature phase-shift keying (QPSK), offset QPSK (OQPSK), and minimum shift keying (MSK) signals transmitted over hard-limited channels in the presence of up-link intersymbol interference (ISI) and CW interference (CWI) is introduced. In the equivalent model the up-link and down-link are interchanged in order to avoid the complicated expectation due to the up-link ISI at the hard-limiter output. The analysis is based on the moment technique and the Gram-Charlier expansion. Numerical results of the BER show that the large bandwidth-symbol time product (BT) or the existence of CWI makes MSK preferable compared with QPSK or OQPSK.     

固体火箭喷管排气中的粒子分布

1.前言 现代的固体火箭发动机为提高推进剂的能量特性及抑制不稳定燃烧，常常在推进剂中添加金属粉末，最常见的是加金属铝粉。在发动机工作时，铝粉燃烧形成凝聚相的氧化铝粒子。这些粒子在喷管中的流动过程中，温度、速度等方面的变化滞后于燃·气本身的变     

On the Detectability and Use of Normal Modes for Determining Interior Structure of Mars

The InSight mission to Mars is well underway and will be the first mission to acquire seismic data from a planet other than Earth. In order to maximise the science return of the InSight data, a multifaceted approach will be needed that seeks to investigate the seismic data from a series of different frequency windows, including body waves, surface waves, and normal modes. Here, we present a methodology based on globally-averaged models that employs the long-period information encoded in the seismic data by looking for fundamental-mode spheroidal oscillations. From a preliminary analysis of the expected signal-to-noise ratio, we find that normal modes should be detectable during nighttime in the frequency range 5–15 mHz. For improved picking of (fundamental) normal modes, we show first that those are equally spaced between 5–15 mHz and then show how this spectral spacing, obtained through autocorrelation of the Fourier-transformed time series can be further employed to select normal mode peaks more consistently. Based on this set of normal-mode spectral frequencies, we proceed to show how this data set can be inverted for globally-averaged models of interior structure (to a depth of \(\sim 250~\mbox{km}\)), while simultaneously using the resultant synthetically-approximated normal mode peaks to verify the initial peak selection. This procedure can be applied iteratively to produce a “cleaned-up” set of spectral peaks that are ultimately inverted for a “final” interior-structure model. To investigate the effect of three-dimensional (3D) structure on normal mode spectra, we constructed a 3D model of Mars that includes variations in surface and Moho topography and lateral variations in mantle structure and employed this model to compute full 3D waveforms. The resultant time series are converted to spectra and the inter-station variation hereof is compared to the variation in spectra computed using different 1D models. The comparison shows that 3D effects are less significant than the variation incurred by the difference in radial models, which suggests that our 1D approach represents an adequate approximation of the global average structure of Mars.     

多层分布式电子监察系统的设计及应用

目前,我国的电子监察系统处于起步阶段,从总体来看,国内电子监察系统的架构设计还不够成熟,主要问题是架构的伸缩性不足、扩展性不足、数据采集方式不灵活。针对这些问题提出了对上述缺点和不足的改进方式,进而设计了"MDES(Multi-layer Distributed Electronic Super-vision System)电子监察系统架构",该架构具有扩展性良好、数据采集方式灵活、数据集中、分布应用等特点,并建立了垂直监管渠道,该架构在佛山市电子监察系统的建设中有了实际的应用,运行情况良好。     

New assignment-based data association for tracking move-stop-move targets

We present a new assignment-based algorithm for data association in tracking ground targets employing evasive move-stop-move maneuvers using ground moving target indicator (GMTI) reports obtained from an airborne sensor. To avoid detection by the GMTI sensor, the targets deliberately stop for some time before moving again. The sensor does not detect a target when the latter's radial velocity (along the line-of-sight from the sensor) falls below a certain minimum detectable velocity (MDV). Even in the absence of move-stop-move maneuvers, the detection has a less-than-unity probability (P/sub D/<1) due to obscuration and thresholding. Then, it is of interest, when a target is not detected, to develop a systematic technique that can distinguish between lack of detection due to P/sub D/<1 and lack of detection due to a stop (or a near stop). Previously, this problem was solved using a variable structure interacting multiple model (VS-IMM) estimator with a stopped target model (VS-IMM-ST) without explicitly addressing data association. We develop a novel "two-dummy" assignment approach for move-stop-move targets that considers both the problem of data association as well as filtering. Typically, in assignment-based data association a "dummy" measurement is used to denote the nondetection event. The use of the standard single-dummy assignment, which does not handle move-stop-move motion explicitly, can result in broken tracks. The new algorithm proposed here handles the evasive move-stop-move motion by introducing a second dummy measurement to represent nondetection due to the MDV. We also present a likelihood-ratio-based track deletion scheme for move-stop-move targets. Using this two-dummy data association algorithm, the track corresponding to a move-stop-move target is kept "alive' during missed detections both due to MDV and due to P/sub D/<1. In addition, one can obtain reductions in both rms estimation errors as well as the total number of track breakages.     

多载波调制结合Turbo编码技术的性能分析

多载波调制是一种有效克服衰落信道频率选择性的技术,从而显著减少码间干扰(ISI)。Turbo码以其接近香农极限的工作性能受到人们的注目,它能在极低信噪比条件下提供可靠通信。把多载波调制与Turbo 编码结合起来能够对整个系统提供显著的性能增益。本文试图对采用这两种技术的通信系统给出性能上的评估。     

火焰筒局部蠕变屈曲分析方法

准确考虑火焰筒温度场和应力场的"局部"特性,提出"局部蠕变屈曲"概念,并给出一套局部蠕变屈曲分析方法.基于Hoff理论建立蠕变屈曲理论模型,结合理论和试验数据验证有限元方法处理蠕变屈曲问题的可行性.考虑蠕变屈曲失稳要素,结合静力结果确定蠕变屈曲危险部位,将子模型技术引入非线性/热弹塑性/蠕变有限元程序中,结合曲率极大点判据,确定危险部位蠕变屈曲临界时间.方法将改善传统方法中的平均温度、平均压应力和平面应变假设,提高了计算精度.      

基于STL文件的笛卡尔网格生成方法研究

采用从STL文件中直接获取模型几何数据的方法,利用ADT数据结构快速剔除相同顶点,提出一种新的“推进查找”方法替代以往网格单元是否在物面内部的判定方法,避免了对物面的自封闭要求,无需进行几何重构,直接完成网格生成,更进一步提高了自适应笛卡尔网格生成速度和自动化程度,为实现CAD与CFD的之间的数据对接提供了一种新的方式。     

A Reverse Monte Carlo Study of H+D Lyman Alpha Absorption from QSO Spectra

A new method based on a Reverse Monte Carlo [RMC] technique and aimed at the inverse problem in the analysis of interstellar (intergalactic) absorption lines is presented. The line formation process in chaotic media with a finite correlation length (l > 0) of the stochastic velocity field (mesoturbulence) is considered. This generalizes the standard assumption of completely uncorrelated bulk motions (l 0) in the microturbulent approximation which is used for the data analysis up-to-now. It is shown that the RMC method allows to estimate from an observed spectrum the proper physical parameters of the absorbing gas and simultaneously an appropriate structure of the velocity field parallel to the line-of-sight.The application to the analysis of the H+D Ly profile is demonstrated using Burles and Tytler [B&T] data for QSO 1009+2956 where the DI Ly line is seen at za = 2.504.The results obtained favor a low D/H ratio in this absorption system, although our upper limit for the hydrogen isotopic ratio of about 4.5 × 10-5 is slightly higher than that of B&T (D/H = 30 _-0.5 ^+0.6 × 10^-5). We also show that the D/H and N(HI) values are, in general, correlated, i.e. the derived D-abundance may be badly dependent on the assumed hydrogen column density. The corresponding confidence regions for an arbitrary and a fixed stochastic velocity field distribution are calculated.     

The split symbol moments SNR estimator in narrow-band channels

The split symbol moments estimator (SSME) is an algorithm that is designed to estimate symbol signal-to-noise ratio (SNR) in the presence of additive white Gaussian noise (AWGN). The performance of the SSME algorithm in bandlimited channels is examined, and the effects of the resulting intersymbol interference (ISI) are quantified. All results obtained are in closed form and can be easily evaluated numerically for performance-prediction purposes. The results are also validated through digital simulations     

Simulation of three-dimensional solar wind disturbances and resulting geomagnetic storms

A kinematic method of representing the three-dimensional solar wind flow is devised by taking into account qualitatively the stream-stream interaction which leads to the formation of a shock pair. Solar wind particles move radially away from the Sun, satisfying the frozen-magnetic field condition. The uniqueness of the present approach is that one can incorporate both theoretical and observational results by adjusting the parameters involved and that a self-consistent data set can be simulated. One can then infer the three-dimensional structure of the solar wind which is vital in understanding the interaction between the solar wind and the magnetosphere, and it is for this reason that the present kinematic method is devised. In the first part of this paper, the present kinematic method is described in detail by demonstrating that the following solar wind features can be simulated: (i) Variations of the solar wind quantities (such as the solar wind speed, the density and the IMF vector), associated with the solar rotation, at the Earth; (ii) the solar wind flow pattern in the meridian planes; (iii) the three-dimensional structure of the corotating interaction region (CIR); and (iv) the three-dimensional structure of the warped solar current sheet.In Section 2, the three-dimensional structure of solar wind disturbances are studied by introducing a flare-generated high speed stream into the two-stream model of the solar wind developed in Section 1. The treatment of the stream-stream interaction is generalized to deal with a flare-generated high speed stream, yielding a shock pair. The shock pair causes three-dimensional distortion of the solar current sheet as it propagates outward from the Sun. It is shown that a set of characteristic time variations of the solar wind speed, density, the interplanetary magnetic field magnitude B and angles (theta) and gf (phi) result at the time of the passage at the location of the Earth for a given set of flare conditions. These quantities allow us to compute the solar wind-magnetosphere energy coupling function . Time variations of the two geomagnetic indices AE and Dst are then estimated from . The simulated geomagnetic storms are compared with observed ones.In the third part, it is shown that recurrent geomagnetic storms can reasonably be reproduced, if fluctuating components of the interplanetary magnetic field (IMF) are superposed on the kinematic model of the solar wind developed in the first part. As an example, we simulate the fluctuating components by linearly polarized Alfvén waves and by random variations of the IMF angle (theta). Characteristics of the simulated and observed geomagnetic storms are discussed in terms of the simulated and observed AE and Dst indices. If the fluctuating components of the IMF can generally be identified as hydromagnetic waves, they may be an important cause for individual magnetospheric substorms, while the IMF magnitude B and the solar wind speed V modulate partially the intensity of magnetospheric substorms and storms.     

The BOOMERANG experiment

The BOOMERANG (Balloon Observations Of Millimetric Extragalactic RAdiation aNd Geophysics) experiment is an international effort to measure the Cosmic Microwave Background (CMB) anisotropy on angular scales of 20 to 4°, with unprecedented sensitivity, sky and spectral coverage. The telescope will be flown from Antarctica by NASA-NSBF with a long duration stratospheric balloon (7–14 days), and is presently scheduled for flight in 1995–1996. The experiment is designed to produce an image of the Cosmic Microwave Background with high sensitivity and large sky coverage. These data will tightly constrain the baryon density, the reionization history, and the formation of large-scale structure in the universe. BOOMERANG will test technologies and return science data that are essential to the design of a future space-borne mission to map CMB anisotropy.     

The Voyager infrared spectroscopy and radiometry investigation

The infrared investigation on Voyager uses two interferometers covering the spectral ranges 60–600 cm^–1 (17–170 m) and 1000–7000 cm^–1 (1.4–10 m), and a radiometer covering the range 8000–25 000 cm^–1 (0.4–1.2 m). Two spectral resolutions (approximately 6.5 and 2.0 cm^–1) are available for each of the interferometers. In the middle of the thermal channel (far infrared interferometer) the noise level is equivalent to the signal from a target at 50 K; in the middle of the reflected sunlight channel (near infrared interferometer) the noise level is equivalent to the signal from an object of albedo 0.2 at the distance of Uranus.For planets and satellites with substantial atmospheres, the data will be used to investigate cloud and gas composition (including isotopic ratios), haze scale height, atmospheric vertical thermal structure, local and planetary circulation and dynamics, and planetary energy balance. For satellites with tenuous atmospheres, data will be gathered on surface and atmospheric composition, surface temperature and thermal properties, local and global phase functions, and surface structure. For Saturn's rings, the composition and radial structure, particle size and thermal characteristics will be investigated. Comparative studies of the planets and their satellite systems will be carried out.Paris Observatory.Cornell University.Jet Propulsion Laboratory.University of Maryland.     

高空长航时无人机结构重量估算方法研究

在对高空长航时无人机总体参数统计数据分析的基础上,利用线性回归分析的方法并结合工程实践经验推导出高空长航时无人机结构重量估算公式;以美国的高空长航时无人机"全球鹰"(global hawk)为例进行估算,结果验证了结构重量评估公式的合理性和可用性;在此评估公式的基础上运用数学方法推导出反映高空长航时无人机总体参数变化与结构重量变化规律的数学公式,并对总体参数的敏感性进行了分析.在飞机总体设计过程中,充分考虑总体设计参数对飞机各部分结构重量的影响规律,就能够使高空长航时无人机结构重量的估算结果更加准确合理.     

OPPORTUNITIES FOR MAGNETOSPHERIC RESEARCH WITH COORDINATED CLUSTER AND GROUND-BASED OBSERVATIONS

ESA's first multi-satellite mission Cluster is unique in its concept of 4 satellites orbiting in controlled formations. This will give an unprecedented opportunity to study structure and dynamics of the magnetosphere. In this paper we discuss ways in which ground-based remote-sensing observations of the ionosphere can be used to support the multipoint in-situ satellite measurements. There are a very large number of potentially useful configurations between the satellites and any one ground-based observatory; however, the number of ideal occurrences for any one configuration is low. Many of the ground-based instruments cannot operate continuously and Cluster will take data only for a part of each orbit, depending on how much high-resolution (burst-mode') data are acquired. In addition, there are a great many instrument modes and the formation, size and shape of the cluster of the four satellites to consider. These circumstances create a clear and pressing need for careful planning to ensure that the scientific return from Cluster is maximised by additional coordinated ground-based observations. For this reason, the European Space Agency (ESA) established a working group to coordinate the observations on the ground with Cluster. We will give a number of examples how the combined spacecraft and ground-based observations can address outstanding questions in magnetospheric physics. An online computer tool has been prepared to allow for the planning of conjunctions and advantageous constellations between the Cluster spacecraft and individual or combined ground-based systems. During the mission a ground-based database containing index and summary data will help to identify interesting datasets and allow to select intervals for coordinated studies. We illustrate the philosophy of our approach, using a few important examples of the many possible configurations between the satellite and the ground-based instruments.     

Galactic and Extragalactic Magnetic Fields

The current state of research of the Galactic magnetic field is reviewed critically. The average strength of the total field derived from radio synchrotron data, under the energy equipartition assumption, is 6±2 G locally and about 10±3 G at 3 kpc Galactic radius. These values agree well with the estimates using the locally measured cosmic-ray energy spectrum and the radial variation of protons derived from -rays. Optical and synchrotron polarization data yield a strength of the local regular field of 4±1 G, but this value is an upper limit if the field strength fluctuates within the beam or if anisotropic fields are present. Pulsar rotation measures, on the other hand, give only 1.4±0.2 G, a lower limit if fluctuations in regular field strength and thermal electron density are anticorrelated along the pathlength. The local regular field may be part of a `magnetic arm between the optical arms. However, the global structure of the regular Galactic field is not yet known. Several large-scale field reversals in the Galaxy were detected from rotation measure data, but a similar phenomenon was not observed in external galaxies. The Galactic field may be young in terms of dynamo action so that reversals from the chaotic seed field are preserved, or a mixture of dynamo modes causes the reversals, or the reversals are signatures of large-scale anisotropic field loops. The Galaxy is surrounded by a thick disk of radio continuum emission of similar extent as in edge-on spiral galaxies. While the local field in the thin disk is of even symmetry with respect to the plane (quadrupole), the global thick-disk field may be of dipole type. The Galactic center region hosts highly regular fields of up to milligauss strength which are oriented perpendicular to the plane. A major extension of the data base of pulsar rotation measures and Zeeman splitting measurements is required to determine the structure of the Galactic field. Further polarization surveys of the Galactic plane at wavelengths of 6 cm or shorter may directly reveal the fine structure of the local magnetic field.     

Thermal radiation from a radio pulsar PSR 1055-52

Conclusion The EXOSAT observation of PSR 1055-52 supports strongly the idea of a thermally radiating neutron star, either still cooling from its initially high temperature or reheated by unpinning of vortex lines in its superfluid interior. The data do not confirm the Cheng & Helfand conclusions about a synchrotron nebula with a power law spectrum. The discrepancy in the data is, nevertheless, only a 3.5 effect, as no ME data could be used to get a firm upper limit of the flux above 1 keV. With regard to the outstanding theoretical interest in the structure of neutron stars we hope for further observations to clarify this question.     

新型变几何火焰稳定器燃烧特性试验

在二元燃烧试验台上研究了一种新型变几何火焰稳定器的燃烧特性,重点描述了在不同试验工况下,稳定器燃烧效率、出口温度分布与稳定器几何形状变化的关系,并且通过稳定器的燃烧图像分析了几何变化对于燃烧状态及火焰结构的影响.结果表明:试验工况下,随着几何形状的改变,稳定器的燃烧效率呈现一定幅度的变化;尾缘槽宽与整流罩宽度比 w/h =1.25表现出其特殊性,在该点稳定器的燃烧状态和火焰结构发生较明显地改变;在稳定燃烧过程中,随着 w/h 的减小,出口截面中心温度不断升高,温度分布的均匀性降低.试验数据和结论有助于加深对该型变几何火焰稳定器的了解,并对该型稳定器的数值模拟和进一步试验研究有着重要的参考意义.      

Coordinated EXOSAT and optical observations of the X-ray burster 4U1735-44

We present the first results of an EXOSAT observation of the low-mass X-ray burster 4U1735-44. The ME data show low-amplitude variations in the persistent flux including two 5% dips separated by 4 hours. The structure of the single observed burst is briefly described. Five hours of simultaneous B-band photometry were obtained at SAAO with 12 minute time resolution; a strong anti-correlation is shown to exist between the X-ray and optical flux, with a high level of significance. A model for this behaviour is suggested, based on reprocessing of the X-ray flux in a corona or stellar wind.