分布式处理在民航生产中的应用

阐述了分布式计算机系统的基本原理以及互连方式,对其功能、特点进行了分析.为使该系统在民航等系统中的应用和研究更加广泛,文中还给出了一些应用实例.     

Local clouds: Distribution, density and kinematics through ground-based and HST spectroscopy

The distribution, kinematics and physical properties of the interstellar matter surrounding the Sun can be inferred from ground-based and UV spectroscopic observations. On a 200 pc scale the local interstellar matter appears inhomogeneous and asymmetric. Although it generally flows towards the lower density region, it is composed of numerous small components a few parsecs in size with slightly different velocities. On a smaller scale the extent and the nature of the Local Cloud which flows over the Sun are discussed based on HST-GHRS observations of nearby stars.     

浅谈如何发挥高校实验室的作用

本文主要阐述了实验的重要性和实验教学的重要地位，实验教学观念转变及实验室如何建设发展，实验室的建设发展对高等院校教学与科研的重要作用，对高等院校的知名度和经济效益，吸引人才等方面起到的推动作用。     

基于排队论的防空部署效率分析

为简化空防对抗中防空部署效率的分析,提出了一种基于排队论的分析方法。将作战过程视为先到先服务的服务系统,在目标持续入侵时目标流作为泊松申请,近、中/远程地空导弹武器集群分别为带失效和有限等待时间的排队系统。在一定的简化条件下建立了两种火力单元部署效率的数学模型。算例表明,该法可描述我方火力单元数、武器系统毁伤能力(服务时间)和空中目标流密度间的关系,能用于评估混编防空武器系统的部署效率,算法简单。     

论“三个代表”思想的时代特点

江泽民同志提出的“三个代表”的重要思想,是站在世纪之交的时代高度,总揽全局,对我党近80年历史经验和50年执政经验的总结,提出了加强执政党自身建设的新思路,创造性地发展了马克思主义党建理论与学说,具有鲜明的时代特点。本文就“三个代表”思想所体现的时代特点进行了初步的探讨,论证了其内在逻辑上的统一性,指出了“三个代表”思想必将成为新世纪党建理论的强大思想武器和伟大旗帜。     

开环全保偏光纤陀螺研究

开环全保偏光纤陀螺结构简单，有使用价值；进入９０年代国外研究成功熔接型保偏光纤耦合器以后，这种陀螺更受重视，向实用方向发展，对研究全保偏光纤陀螺中的几个关键问题，光路中元器件的特性；保偏光纤的对轴熔接技术，零漂和噪声做了分析，实验结果表明，零漂达到１．２４°／ｈ。     

Quasi-biennial oscillations in the cross-correlation of properties of macrospicules

Jets, whatever small (e.g. spicules) or large (e.g. macrospicules) their size, may play a key role in momentum and energy transport from photosphere to chromosphere and at least to the low corona. Here, we investigate the properties of abundant, large-scale dynamic jets observable in the solar atmosphere: the macrospicules (MS). These jets are observationally more distinct phenomena than their little, and perhaps more ubiquitous, cousins, the spicules. Investigation of long-term variation of the properties of macrospicules may help to a better understanding of their underlying physics of generation and role in coronal heating. Taking advantage of the high temporal and spatial resolution of the Solar Dynamics Observatory, a new dataset, with several hundreds of macrospicules, was constructed encompassing a period of observations over six years. Here, we analyse the measured properties and relations between these properties of macrospicules as function of time during the observed time interval. We found that cross-correlations of several of these macrospicule properties display a strong oscillatory pattern. Next, wavelet analysis is used to provide more detailed information about the temporal behaviour of the various properties of MS. For coronal hole macrospicules, a significant peak is found at around 2-year period. This peak also exists partially or is shifted to longer period, in the case of quiet Sun macrospicules. These observed findings may be rooted in the underlying mechanism generating the solar magnetic field, i.e. the global solar dynamo.     

New insights into SNR evolution revealed by the discovery of recombining plasmas

We report the discovery of recombining plasmas in three supernova remnants (SNRs) with the Suzaku X-ray astronomy satellite. During SNR’s evolution, the expanding supernova ejecta and the ambient matter are compressed and heated by the reverse and forward shocks to form an X-ray emitting hot plasma. Since ionization proceeds slowly compared to shock heating, most young or middle-aged SNRs have ionizing (underionized) plasmas. Owing to high sensitivity of Suzaku, however, we have detected radiative recombination continua (RRCs) from the SNRs IC 443, W49B, and G359.1–0.5. The presence of the strong RRC is the definitive evidence that the plasma is recombining (overionized). As a possible origin of the overionization, an interaction between the ejecta and dense circumstellar matter is proposed; the highly ionized gas was made at the initial phase of the SNR evolution in dense regions, and subsequent rapid adiabatic expansion caused sudden cooling of the electrons. The analysis on the full X-ray band spectrum of IC 443, which is newly presented in this paper, provides a consistent picture with this scenario. We also comment on the implications from the fact that all the SNRs having recombining plasmas are correlated with the mixed-morphology class.     

The damping of small-amplitude oscillations in quiescent prominences

The presence of small-amplitude oscillations in prominences is well-known from long time ago. These oscillations, whose exciters are still unknown, seem to be of local nature and are interpreted in terms of magnetohydrodynamic (MHD) waves. During last years, observational evidence about the damping of these oscillations has grown and several mechanisms able to damp these oscillations have been the subject of intense theoretical modelling. Among them, the most efficient seem to be radiative cooling and ion-neutral collisions. Radiative cooling is able to damp slow MHD waves efficiently, while ion-neutral collisions, in partially ionised plasmas like those of solar prominences, can also damp fast MHD waves. In this paper, we plan to summarize our current knowledge about the time and spatial damping of small-amplitude oscillations in prominences.     

Modeling Pulsar Wind Nebulae

In the last few years, new observations by CHANDRA and XMM have shown that Pulsar Wind Nebulae present complex but similar inner features, with the presence of axisymmetric rings and jets, which are generally referred to as a jet-torus structure. Due to the rapid growth in accuracy and robustness of numerical schemes for relativistic fluid-dynamics, it is now possible to model the flow and magnetic structure of the relativistic plasma responsible for the emission. Recent results have clarified how the jet and rings are formed, suggesting that the morphology is strongly related to the wind properties, so that, in principle, it is possible to infer the conditions in the unshocked wind from the nebular emission. I will review here the current status in the modeling of Pulsar Wind Nebulae, and, in particular, how numerical simulations have increased our understanding of the flow structure, observed emission, polarization and spectral properties. I will also point to possible future developments of the present models.