"神舟二号"大气密度探测器的探测结果Ⅱ.在太阳和地磁扰动期间高层大气密度的变化

选用了Sz—2大气密度探测器在2001年2—4月间的探测数据,进行日照和阴影区域热层大气密度对太阳和地磁活动程度的响应变化的探讨．结果表明,日照区大气密度峰值主要随F10.7值而变,在地磁扰动期间,阴影区大气密度对扰动的响应更明显,通常响应变化开始于高纬度地区,然后向低纬度地区推移．     

应用关联规则构建质量活动链模型

介绍了作业质量成本的概念,提出了以作业质量成本数据为基础描述质量活动间关联关系的方法,并设定了作业质量成本之间相互影响的规则.着重研究了关联规则挖掘技术,将布尔型关联规则用于质量活动间作用关系的挖掘,并应用Apriori算法,研究了应用作业质量成本数据及其变化趋势构建基于作业质量成本的质量活动链模型的方法.该模型有助于在质量成本预测与分析过程中从经济的角度发现质量管理过程的瓶颈问题,为以质量成本分析为基础,系统地进行质量改进决策提供了有效的方法和手段.      

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.     

Soft X-Ray and Extreme Ultraviolet Excess Emission from Clusters of Galaxies

An excess over the extrapolation to the extreme ultraviolet and soft X-ray ranges of the thermal emission from the hot intracluster medium has been detected in a number of clusters of galaxies. We briefly present each of the satellites (EUVE, ROSAT PSPC and BeppoSAX, and presently XMM-Newton, Chandra and Suzaku) and their corresponding instrumental issues, which are responsible for the fact that this soft excess remains controversial in a number of cases. We then review the evidence for this soft X-ray excess and discuss the possible mechanisms (thermal and non-thermal) which could be responsible for this emission.     

Simulation Techniques for Cosmological Simulations

Modern cosmological observations allow us to study in great detail the evolution and history of the large scale structure hierarchy. The fundamental problem of accurate constraints on the cosmological parameters, within a given cosmological model, requires precise modelling of the observed structure. In this paper we briefly review the current most effective techniques of large scale structure simulations, emphasising both their advantages and shortcomings. Starting with basics of the direct N-body simulations appropriate to modelling cold dark matter evolution, we then discuss the direct-sum technique GRAPE, particle-mesh (PM) and hybrid methods, combining the PM and the tree algorithms. Simulations of baryonic matter in the Universe often use hydrodynamic codes based on both particle methods that discretise mass, and grid-based methods. We briefly describe Eulerian grid methods, and also some variants of Lagrangian smoothed particle hydrodynamics (SPH) methods.     

前苏联可靠性工程的几个特点

与美，英体系相比、前苏联可靠性工程独具特点，对可靠性保证概念；可靠性工程与产品故障机理分析相结合；可靠性分析与系统功能分析相结合；可靠性工程与相关学科相结合；注重工程实用与ＣＡＤ化等五个方面进行了阐述，并强调了研究和借鉴前苏联可靠性工程的重要性。     

PSD器件及其在精密测量中的应用

ＰＳＤ器件是近几年出现的一种新型位置探测器，可直接用来测量角度、高度、距离及运动，本文介绍了ＰＳＤ器件的工作，给出了三种ＰＳＤ器件的等电路和坐标位置电流函数表达式，并就ＰＳＤ器件在位移和三维运动测量中应用方式和应用范围进行了讨论。     

超音通流风扇叶栅流场数值模拟

用矢通量分裂法求解Ｎ－Ｓ方程和Ｅｕｌｅｒ方程，对超音通流风扇叶栅流场进行了数值模拟，由计算结果给出的物理图象表明，叶栅通道内没有强激波，亦未出现分离回流，全叶栅流场均为超音速，说明计算的两种叶型符合设计要求，其性能有待实验检验。     

Bi_(1.9)Pb_(0.3)Sr_(2.0)Ca_(1.7)Mg_(0.3)Cu_(3.1)O_x 超导块材弱连接区的低磁场性

通过对在不同外磁场下Ｂｉ１．９Ｐｂ０．３Ｓｒ２．０Ｃａ１．７Ｍｇ０．３Ｃｕ３．１Ｏｘ超导块材的交流磁化率的测量，获得了样品内晶粒间和晶粒内对外场的不问响应范围．通过与粉状样品实验结果的比较和Ｘ光分析，认为块状样品在温度为１００Ｋ左右出现的抗磁台阶是样品内晶粒间超导弱连接的一种抗磁效应．对弱连接区有效钉扎力Ｆｐ和临界电流密度Ｊｃ与外场Ｈ的关系进行了讨论．     

Report on the Kiso cometary dust trail survey

Cometary dust trails were first observed by IRAS; they are widely known to be the origins of meteoric showers. A new window has been opened for the study of dust trails, using ground-based observations. We succeeded in obtaining direct images of the 22P/Kopff dust trail with the Kiso 1.05-m Schmidt telescope. Following this initial success, we have continued to perform a dust trail survey at Kiso. As a result of this survey, we have detected dust trails along the orbit of six periodic comets, between February 2002 and March 2004. The optical depth of these dust trails are 10⁻⁹ to 10⁻⁸, which is consistent with IRAS measurements. In this paper, we describe the observations and data reduction procedures, and report the brief result obtained between February 2002 and March 2004.