First millimetric detections of AE Aquarii

We report the first millimetric detections of the magnetic cataclysmic variable AE Aquarii, accompanied by contemporaneous microwave observations. These data show that the time-averaged spectrum is well fit by a power-law which extends to mm wavelengths. We suggest that the spectrum is consistent with that expected from a superposition of flare-like events.     

Observational Signatures of Particle Acceleration in Supernova Remnants

We evaluate the current status of supernova remnants as the sources of Galactic cosmic rays. We summarize observations of supernova remnants, covering the whole electromagnetic spectrum and describe what these observations tell us about the acceleration processes by high Mach number shock fronts. We discuss the shock modification by cosmic rays, the shape and maximum energy of the cosmic-ray spectrum and the total energy budget of cosmic rays in and surrounding supernova remnants. Additionally, we discuss problems with supernova remnants as main sources of Galactic cosmic rays, as well as alternative sources.     

X-ray Reflection

Material irradiated by X-rays produces backscattered radiation which is commonly known as the Reflection Spectrum. It consists of a structured continuum, due at high energies to the competition between photoelectric absorption and electron scattering enhanced at low energies by emission from the material itself, together with a complex line spectrum. We briefly review the history of X-ray reflection in astronomy and discuss various methods for computing the reflection spectrum from cold and ionized gas, illustrated with results from our own work reflionx. We discuss how the reflection spectrum can be used to obtain the geometry of the accretion flow, particularly the inner regions around black holes and neutron stars.     

二维三角晶格的Peierls相变前后的声子色散曲面的研究

利用晶格动力学理论计算了二维三角晶格的Peierls相变前后的声子能谱。并且在第一布里渊区绘制了声子色散曲面。通过对Peierls相变前后的声子能谱比较可知，随其对称性降低，声子能谱的简并度被破缺。二维三角晶格的Peierls相变前只有两支声频支声子能谱，Peierls相变后有两支声频支声子能谱与两支光频支声子能谱，并且声频支声子能谱与光频支声子能谱不相交，两支光频支声子沿ky轴平缓地变化。     

二维三角晶格的Peierls相变前后的声子色散曲线的研究

利用品格动力学理论计算了二维三角品格的Peimrls相变前后的声子能谱。并且在第一布里渊区绘制了主要的对称点、线上的声子色散曲线。通过对Peierls相变前后的声子能谱比较可知，随其对称性降低，声子能谱的简并度被破缺。二维三角品格的Peierls相变前只有两支声频支声子能谱，Peierls相变后有两支声频支声子能谱与两支光频支声子能谱，并且声频支声子能谱及光频支声子能谱不相交，两支光频支声子沿ky轴平缓地变化。     

Identification of a 2D turbulent wind spectrum

Turbulent wind spectrum models usually involve nonrational terms. For such models the development of a Markovian time simulator relies on a rational approximation obtained by the way of an identification stage. This paper presents a general method to manage this identification stage, that provides us with a family of stable rational approximations which is proved to converge towards the true model as the dimension increases. We first give an exact but infinite dimensional state space representation of the spectrum. It is based on the use of a diffusive equation. For bi-dimensional (2D) signals it also uses decoupling by spatial Fourier transformation. Then the discretization of this exact model leads easily to stable finite dimensional approximations over a prescribed frequency range. This approach is applied to the identification of a theoretical 2D turbulent wind spectrum, and of a 1D turbulent wind spectrum estimated from in flight recorded data.     

谱载荷作用下的疲劳裂纹扩展寿命

本文根据过载迟滞效应中产生推迟延缓的机理,得出了计算推迟延缓参数的公式。提出了对拉伸过载和拉-压过载作用下的裂纹扩展计算模型。用本模型可以计算复杂谱载荷作用下的疲劳裂纹扩展寿命。本文计算了几种材料在不同加载条件下的迟滞效应。计算了飞机机翼加劲板和飞机起落架旋转臂在复杂谱载荷作用下的疲劳裂纹扩展寿命。计算结果与实验结果相当符合。     

扩频时隙ALOHA技术捕捉能力及性能分析

在传统的时隙ALOHA随机多址技术的基础上,提出了与DS/SS-CDMA结合的扩频时隙ALOHA技术,主要对其捕捉性能进行了分析,并且引入马尔可夫模型以便探讨它的吞吐量和时延等参数。     

Modeling Multifractality of the Solar Wind

The question of multifractality is of great importance because it allows us to investigate interplanetary hydromagnetic turbulence. The multifractal spectrum has been investigated with Voyager (magnetic field) data in the outer heliosphere and with Helios (plasma) data in the inner heliosphere. We use the Grassberger and Procaccia method that allows calculation of the generalized dimensions of the solar wind attractor in the phase space directly from the cleaned experimental signal. We analyze time series of plasma parameters of the low-speed streams of the solar wind measured in situ by Helios in the inner heliosphere. The resulting spectrum of dimensions shows a multifractal structure of the solar wind attractor. In order to quantify that multifractality, we use a simple analytical model of the dynamical system. Namely, we consider the generalized self-similar baker’s map with two parameters describing uniform compression and natural invariant measure on the attractor of the system. The action of this map exhibits stretching and folding properties leading to sensitive dependence on initial conditions. The obtained solar wind singularity spectrum is consistent with that for the multifractal measure on the weighted baker’s map.     

Robust detection of small stochastic signals

We consider the problem of detecting a stochastic signal in white not-necessarily-Gaussian noise, using vector valued observations. The locally optimal detector is presented and its performance evaluated. The least-favorable signal spectrum and noise density (over specified classes) are found, and it is shown that the detector using these least-favorable assumptions is minimax robust. The class of spectra is that of any stochastic signal of specified power whose spectrum can be bounded from above and from below by two given positive functions. The class of densities is the ε-contamination model. We present examples of the performance achievable with the robust detector in one of these the spectral uncertainty class corresponds to the unknown Doppler shift of a radar return signal. It is demonstrated that the standard matched-filter's performance degradation with increasing Doppler shift can be avoided almost entirely through use of the robust processor     

The X-ray and optical variability of the BLRG 3C390.3

We describe the optical emission line and continuum changes in 3C390.3. Also we present new EXOSAT results, and discuss their implication for determination of the X-ray spectrum — spectral index and absorbing column.     

Signatures of Coronal Hole Spectra Between 660 Å and 1460 Å Measured with Sumer on Soho

Spectra of the northern polar coronal hole measured with the SUMER spectrometer on SOHO on 25 October 1996 are analyzed. We present spectra taken at locations on the solar disk where part of the spectrometer slit intersects a polar coronal hole region and an area of brighter emission from outside of the coronal hole area. By comparing the line intensities between the parts of the spectrum taken inside the "dark" area of the coronal holes and the brighter regions, we work out the signatures of the specific coronal hole in the chromosphere, transition region and lower corona. We find that emissions of neutral atom lines, of which there are many in the spectrum of SUMER, show no difference between the coronal hole and the bright boundary areas, whereas all ionized species show strong intensity enhancements, including the continuum emissions of carbon and hydrogen. These enhancements are larger than in normal quiet Sun areas. This revised version was published online in June 2006 with corrections to the Cover Date.     

The role of antiprotons in cosmic-ray physics

Though success eluded experimentalists from detecting cosmic-ray antiprotons over a long period of time, the study of cosmic-ray antiprotons has now become a fascinating field of research. In this review, we have attempted to elucidate the excitement in this area of research since the discovery of antiprotons in the laboratory. We have described the experiments carried out so far to measure the energy spectrum of antiprotons, from about 200 MeV to about 15 GeV, and summarised the results. The observed spectrum, with the limited data, appears to be very hard and is different from other components of cosmic radiation. Upper limits to the fraction of antiprotons in cosmic-rays have also been derived at higher energies, using the observed spectra of cosmic-ray primary and secondary particles at different depths in the atmosphere. We have described various physical processes by which antiprotons could be produced, such as high-energy interactions, neutron oscillations, evaporation of Mini Black Holes, decay of super symmetric particles, etc. The energy spectrum of antiprotons, which are produced through the above processes, undergoes modifications during propagation in the Galaxy. We have examined in detail the propagation models which have been employed to explain the observed data. It is shown that no single model could predict correctly the observed energy spectrum of antiprotons over the entire energy region. However, many models are able to explain the data at relativistic energies. It is difficult at this stage to make a choice among these models. The implications of these models for other components of cosmic-rays, such as positrons, deuterium, and He, have been discussed. We have examined the production of gamma rays in the Galaxy from sources, which produce the observed antiprotons through high-energy interactions. We have also briefly indicated the effect of possible re-acceleration during their confinement in the Galaxy. We finally emphasized the need for more detailed measurements of the spectral shape of cosmic-ray antiprotons to further refine speculations of their origin. Similarly, we have shown that detailed observation of the energy spectra of positrons, deuterium, and He at relativistic energies are crucial to test various propagation models.     

Improved algorithm for estimating pulse repetition intervals

This paper presents an improved algorithm for estimating pulse repetition intervals (PRIs) of an interleaved pulse train which consists of several independent radar signals with different PRIs. The original version of this algorithm is a complex-valued autocorrelation-like integral, which leads to a kind of PRI spectrum wherein the locations of the spectral peaks indicate the PRI values. The original algorithm, however, has a serious drawback in that it is vulnerable to timing jitter (PRI jitter). We analyze the cause of this vulnerability and propose an improved algorithm using overlapped PRI bins which have shifting time origins. The improved algorithm has proven to be quite effective in obtaining the PRI spectrum for jittered pulse trains, which enables detection of mean PRIs by thresholding     

复杂电磁环境下频谱智能管控技术探讨

作为国土空间的重要组成,电磁频谱空间呈现出环境错综复杂、目标类型多样、用频行为多变等新挑战,导致频谱安全问题日益严峻。面向复杂电磁环境下频谱秩序安全、频谱对抗安全和频谱共享安全等需求,基于人工智能的频谱管控成为电磁频谱领域的重要研究方向,存在着具有挑战性的基础理论问题和关键技术难题。首先,调研了复杂电磁环境下频谱智能管控的国家战略需求,然后,提炼了智能频谱管控的科学意义与技术挑战,进一步从频谱管控模型机理、频谱态势感知、频谱行为推理、频谱安全决策和频谱管控应用系统等5个方面梳理国内外研究现状,并分析了相关发展动态及研究趋势。     

High energy neutrinos from quasars

We review and clarify the assumptions of our basic model for neutrino production in the cores of quasars, as well as those modifications to the model made subsequently by other workers. We also present a revised estimate of the neutrino background flux and spectrum obtained using more recent empirical studies of quasars and their evolution. We compare our results with other theoretical calculations and experimental upper limits on the AGN neutrino background flux. We also estimate possible neutrino fluxes from the jets of blazars detected recently by the EGRET experiment on the Compton Gamma Ray Observatory. We discuss the theoretical implications of these estimates.NAS-NRC Senior Research Associate, on leave from the Physics Department, University of Utah     

基于实测数据的疲劳寿命分散系数取值研究

随着基准谱、严重谱编制研究的深入,利用实测数据编制载荷谱在编谱方法和分散系数取值等方面需 求愈发迫切。从正态概率分布理论出发,讨论影响疲劳寿命分散系数取值的主要因素;针对基准谱和严重谱之 间的差异性,提出基准谱和严重谱的折算思路和方法,并通过实测数据编制的基准谱和严重谱折算系数进行比 较分析。结果表明：采用本文方法可以实现基准谱与严重谱之间损伤分散系数的折算取值。     

基于ap-Welch的随机角振动信号的 频谱估计方法研究

在转台的随机角振动试验中,频谱估计的精度是一个非常重要的指标,直接影响到频谱复现的精度.在分析经典的频谱估计方法的基础上,提出了一种基于ap-Welch频谱估计(基于全相位预处理的Welch频谱估计)的方法,从理论上证明了其比Welch频谱估计法具有更强的旁瓣抑制作用.仿真实验结果表明,ap-Welch频谱估计法能够有效提高频谱估计的精度,而且随着全相位阶数的增加,频谱估计的收敛特性也随之改善.     

Extreme solar cycle variability in strong lines between 200 and 400 NM

Our study of solar cycle irradiance variability in the UV between 200 and 400 nm requires a detailed knowledge of the composition of the solar spectrum in this wavelength range. We compute the synthetic spectrum from 250 to 300 nm and compare it with ATLAS3 and SOLSTICE observations. Synthetic solar spectra for solar minimum and maximum conditions show large variations in broad, strong UV lines. Strong lines of FeI between 260 nm and 264 nm show increases between 0.4× and 3×in their max/min ratio. Our ``broad lines' database shows 167 lines with similar properties between 200 nm and 400 nm. Our results raise issues of the importance of such large variability in narrow bands and the difficulty of detection in measurements with spectral resolutions of 1 nm.     

晶格常数对亚铁磁性二维长方晶格磁振子能谱的影响

利用Heisenberg交换作用模型、格林函数法研究了X-Y-Z模型亚铁磁性Heisenberg系统下的二维长方复式晶格的自旋波解。并且讨论了系统的磁振子能谱随交换积分常数比J2 /J1的变化规律,以及在第一布里渊区中的 线上随波矢k 的变化规律。因为交换积分(J1, J2 )与亚铁磁性晶体的晶格常数有关, 并且随晶格常数的增加交换积分 (J1, J2 )将减小。我们得出系统的磁振子能谱在∑线分裂为E4 >E2 >0>E1 >E3,并且E1、E3 随晶格常数的减小而减小,但是E2、E4 随晶格常数的减小而增大。