The Cassini Cosmic Dust Analyzer

The Cassini-Huygens Cosmic Dust Analyzer (CDA) is intended to provide direct observations of dust grains with masses between 10⁻¹⁹ and 10⁻⁹ kg in interplanetary space and in the jovian and saturnian systems, to investigate their physical, chemical and dynamical properties as functions of the distances to the Sun, to Jupiter and to Saturn and its satellites and rings, to study their interaction with the saturnian rings, satellites and magnetosphere. Chemical composition of interplanetary meteoroids will be compared with asteroidal and cometary dust, as well as with Saturn dust, ejecta from rings and satellites. Ring and satellites phenomena which might be effects of meteoroid impacts will be compared with the interplanetary dust environment. Electrical charges of particulate matter in the magnetosphere and its consequences will be studied, e.g. the effects of the ambient plasma and the magnetic field on the trajectories of dust particles as well as fragmentation of particles due to electrostatic disruption.The investigation will be performed with an instrument that measures the mass, composition, electric charge, speed, and flight direction of individual dust particles. It is a highly reliable and versatile instrument with a mass sensitivity 10⁶ times higher than that of the Pioneer 10 and 11 dust detectors which measured dust in the saturnian system. The Cosmic Dust Analyzer has significant inheritance from former space instrumentation developed for the VEGA, Giotto, Galileo, and Ulysses missions. It will reliably measure impacts from as low as 1 impact per month up to 10⁴ impacts per second. The instrument weighs 17 kg and consumes 12 W, the integrated time-of-flight mass spectrometer has a mass resolution of up to 50. The nominal data transmission rate is 524 bits/s and varies between 50 and 4192 bps.This revised version was published online in July 2005 with a corrected cover date.     

37kW底盘测功机计算机控制系统

底盘测功机是检验汽车、摩托车输出功率及其相关参数的一种检测设备。本课题利用现代先进的计算机控制技术实现对37kW-CHDY底盘测功机的行驶阻力控制、测试数据自动采集,从而实现摩托车道路工况模拟运转以及整车动力性、燃料经济性等指标的测量。     

混合气体流动的一种数值模拟方法

本文建立一个数值模拟完全气体混合流动的理论模型.该模型首先应用混合气体的Euler方程和每种气体组分的质量分数方程来控制流动.为了消除混合网格内气体组分界面附近出现的非物理振荡,我们假定混合气体的每种组分达到了动力学平衡状态然而尚未达到热力学平衡状态.这种思想导致需要另外给定每种气体组分的总能量方程.为使用高分辨格式来求解这组双曲型偏微分方程并且简化对所需要的Jacobi矩阵的推导,混合气体的压力方程也被耦合起来.Godunov型的波传播方法被采用来离散求解所获得的控制方程.从典型算例结果来看,一维问题的数值解与精确解一致,二维问题的数值解与理论分析一致.这说明本文的理论模型是合理的.     

细长旋成体大迎角绕流的背涡结构与压力脉动特性

在亚临界流动范围内,通过尖拱细长旋成体在无侧滑状态下的脉动压力测量,对大迎角下细长旋成体非对称背涡结构沿轴向的压力脉动特征进行了研究分析,揭示了压力的脉动幅度与频率沿旋成体轴向的变化规律及其与背涡结构之间的对应关系,并对压力脉动特征沿轴变化的原因进行了初步探讨.     

瓦状特征型面塞式喷管三维计算与实验

为了进一步了解瓦状塞式喷管的性能,采用NND差分格式求解三维N S方程和空气冷流对6单元瓦状特征型面塞式喷管进行了数值模拟和实验研究。研究模型的内喷管面积比为4,总面积比为40,设计压强比为1047。计算得到了流场马赫数和塞锥表面压强分布、喷管推力系数效率,以及不同压强比下中心平面、过渡平面和边缘平面的塞锥表面压强变化规律。计算结果与实验数据吻合得较好,效率数值最大相差1%。实验塞式喷管最大的推力系数效率为0 995,同钟型喷管相比,具有很好的高度补偿能力:从地面到高空,效率在0 93～0 995之间变化。和以前简化型面的4单元瓦状塞式喷管相比,实验和数值模拟均说明塞锥特征型面的优化设计提高了喷管性能,更充分体现了塞式喷管的高度补偿特性,可以成为未来工程应用的选择方案。     

试论我国财务软件服务体系的建立

我国财务软件发展至今,总体上看还很不健全,针对实践中遇到的问题,对财务软件服务体系的建立做一些实证性上的探讨。     

2.5D石英纤维织物增强二氧化硅基复合材料弯曲性能测试研究

简要介绍了2．5D石英纤维织物增强二氧化硅基复合材料弯曲性能测试装置，通过对比试验研究了试样跨厚比、变形测量等对材料弯曲性能的影响，用数理统计的方法对总体均值进行了显著性检验，合理确定了材料弯曲性能测试的试验参数。     

TC6钛合金棒材热处理工艺研究

对TC6钛合金φ20mm～φ120mm不同规格棒材进行了普通退火、双重退火、等温退火、固溶时效等热处理方法和热处理制度研究,并对比分析了热处理制度和组织、性能之间的影响关系,结果表明,TC6钛合金的组织和性能对热处理工艺敏感,应根据半成品规格、类型、截面形状、使用温度、受力情况以及设备条件等诸多因素选择合适的热处理方法和制度,才能达到强度、塑性和韧性的最佳匹配。研究结果证实普通退火是一种简单易行的退火制度,适用于飞机结构用中等规格棒材等半成品的退火,进一步提出了TC6钛合金棒材的热处理工艺选择原则。     

The Solar and Cosmic-Ray Synodic Periodicity (1969–1998)

The synodic recurrence of the Mt. Wilson plage index (MPSI) and the Calgary cosmic ray (CR) intensity is investigated, using the wavelet power spectra in the range of 18–38 days, during the last three solar cycles. The unique temporal coincidence between the quasi–synodic MPSI and the CR periods is detected in 1978–1982 (the 21st solar cycle). In the 22nd cycle there is a very strong MPSI synodic recurrence, from 1989.5 to 1990.5, but it is absent in the CR data. In 1992.5–1993.5 the MPSI and CR recurrence phenomenon is in good accordance with the solar wind speed and cosmic ray modulation as measured during the first Ulysses passage around the Sun. The Gnevyshev gap is present in the 27-day recurrence of CR, in agreement with Kudela et al. (1999). This revised version was published online in August 2006 with corrections to the Cover Date.     

The Time-of-Flight Energy,Angle, Mass Spectrograph (Teams) Experiment for Fast

The Time-of-flight Energy Angle Mass Spectrograph (TEAMS) is being flown on the FAST Small Explorer mission to measure the 3-dimensional distribution function of the major ion species present in the lower magnetosphere. The instrument is similar to time-of-flight plasma analyzer systems that have been designed and planned for flight as CODIF (COmposition and DIstribution Function analyzer) on the four European Space Agency Cluster-II spacecraft and, as ESIC (Equator-S Ion Composition instrument) on Equator-S. This instrument allows the 3-dimensional distribution functions of individual ion species to be determined within spin period (2.5 s). Two-dimensional distributions are measured in 80 ms. These capabilities are crucial for the study of selective energization processes in the auroral regions of the magnetosphere. The design, operational characteristics, and test and calibration results for this instrument are presented. The sensor consists of a toroidal top-hat electrostatic analyzer with instantaneous acceptance of ions over 360° in polar angle. After post-acceleration of the incoming ions by up to 25 kV, a time-of-flight mass spectrograph discriminates the individual species. It has been demonstrated through calibration that the instrument can easily separate H⁺, He²⁺, He⁺, O⁺ and, for energies after post-acceleration of > 20 keV, even O₂ ⁺ molecules. On-board mass discrimination and the internal accumulation of several distinct data quantities combined with the spacecraft's flexible telemetry formatting allow for instrument data rates from 7.8 kb s^–1 to 315 kb s^–1 to be telemetered to ground through the FAST centralized Instrument Data Processor.