扫描辐射计内光路反射镜中SiO2／Ag薄膜系统的失效分析

SiO_2/Ag薄膜系统是扫描辐射计内光路反射镜的主要组成部分。采用高分辨扫描俄歇微探针(SAM)和扫描电镜分析对SiO_2/Ag 薄膜系统失效进行了较为全面的分析研究。通过扫描电镜观察发现,失效的反射镜表面SiO_2薄膜上存在大量析出物,借助于SAM分析,表明这些析出物主要是银和铜,析出物表面伴随有硫化和氧化。SAM的深度剖面结果说明,有析出物存在的区域,各薄膜层中存在原子间的扩散。文章就反射镜中Ag、Cu、和O的扩散和穿透行为进行了讨论,认为SiO_2薄膜致密度较差是导致反射镜失效的主要原因之一。     

漏极注入HPM对高电子迁移率晶体管的损伤机理

针对典型GaAs高电子迁移率晶体管（HEMT）低噪声放大器,利用半导体仿真软件Sentaurus-TCAD建立了HEMT低噪声放大器二维电热模型,考虑高电场下的载流子迁移率退化和载流子雪崩产生效应,分析了由漏极注入高功率微波(HPM)情况下器件内部的瞬态响应,通过分析器件内部电场强度、电流密度、温度分布随信号作用时间的变化,研究了其损伤效应与机理。研究结果表明,当漏极注入幅值17.5V、频率为14.9GHz的微波信号后,峰值温度随信号作用时间的变化呈现周期性“增加—减小—增加”的规律。在正半周期降温,在负半周期升温,总体呈上升趋势,正半周电场峰值主要出现在漏极,负半周电场峰值主要出现在栅极靠漏侧,端电流在第二周期之后出现明显的双峰现象。由于热积累效应,栅极下方靠漏侧是最先发生熔融烧毁的部位,严重影响了器件的可靠性,而漏极串联电阻可以有效提高器件抗微波损伤能力。最后,对微波信号损伤的HEMT进行表面形貌失效分析,表明仿真与试验结果基本相符。     

漏极注入HPM对高电子迁移率晶体管的损伤机理

针对典型GaAs高电子迁移率晶体管(HEMT)低噪声放大器,利用半导体仿真软件Sentaurus-TCAD建立了HEMT低噪声放大器二维电热模型,考虑高电场下的载流子迁移率退化和载流子雪崩产生效应,分析了由漏极注入高功率微波(HPM)情况下器件内部的瞬态响应,通过分析器件内部电场强度、电流密度、温度分布随信号作用时间的变化,研究了其损伤效应与机理。研究结果表明,当漏极注入幅值17.5V、频率为14.9GHz的微波信号后,峰值温度随信号作用时间的变化呈现周期性"增加—减小—增加"的规律。在正半周期降温,在负半周期升温,总体呈上升趋势,正半周电场峰值主要出现在漏极,负半周电场峰值主要出现在栅极靠漏侧,端电流在第二周期之后出现明显的双峰现象。由于热积累效应,栅极下方靠漏侧是最先发生熔融烧毁的部位,严重影响了器件的可靠性,而漏极串联电阻可以有效提高器件抗微波损伤能力。最后,对微波信号损伤的HEMT进行表面形貌失效分析,表明仿真与试验结果基本相符。     

考虑低能电子影响的二次电子修正模型

随着微放电效应研究的不断深入,低能电子影响在微放电过程中越来越不可忽视。当前常用的微放电模型在处理低能电子问题上具有一定的局限性,为了精确模拟这一过程,在深入研究二次电子和背散射电子发射理论的基础上,分别针对材料表面条件不同引起的二次电子发射系数不确定性、低能电子的背散射系数以及电子入射角等问题进行了分析和讨论,并在此基础上建立了一个二次电子发射模型,最后通过数值计算讨论了模型的正确性和适用范围。这一模型同时考虑材料表面条件参数、低能电子的背散射系数以及入射角等因素影响,能够兼容较低能量电子的二次发射,提升微放电数值模拟的精确度和适用性,为微放电数值模拟的发展起到推进作用。     

机械失效模式、原因和机理的诊断思路和主要依据

从断口、裂纹、痕迹和参数等4个方面阐述了机械失效模式、原因和机理诊断的主要依据,列出了机械使用失效的主要模式、原因和失效的主要形成条件和主要的诊断思路,并从单项分析和综合分析的角度给出了失效模式、原因和机理诊断所需要的"多维"信息系统,为分析和确认各种失效模式、原因和机理提供了主要的推理规则和基本方法;最后分析比较了各种二级疲劳失效模式和各种与应力腐蚀有关的失效模式之间的主要诊断依据和应注意的几个问题,为疑难二级失效模式的诊断问题提供了分析研究方向.      

直流微电流标准源

一、概述微电流测试仪的最高分辨力已达10~(-17)A,不确定度在百分之几数量级。用于校准微电流测试仪器的微电流源主要有三种类型:电阻式、电容式和电离式。电阻式直流微电流源由可调参考电压源和一系列高阻组成,具有结构简单和能持续输出(t—∞)的优点,但由于高阻的稳定性差,这种微电流源的不确定度不太高。目前,电阻式微电流源在10~(-13)A输出时,不确定度只能达到百分之几数量级。电容式微电流源以线变电压发生器和微分电容为基础,采用微分线变电压原理实现微小电流输出。这种微电流源在10~(-13)A     

多种失效模式履带车辆扭力轴可靠性稳健设计

履带车辆扭力轴通常存在多种失效模式,因此对其进行灵敏度设计分析时需要充分考虑不同失效模式的影响。提出一种多失效模式机械零件可靠性灵敏度分析的数值方法,运用随机摄动理论和四阶矩技术,求得各个失效模式状态函数的前四阶矩和可靠性指标,有效解决了结构随机变量参数分布未知时,不同失效模式下构件可靠度的计算问题。根据机械零件发生一种失效模式即整体失效的具体特点,研究含相关性的不同失效模式机械零件的可靠度计算方法。结合灵敏度分析的梯度算法,推导出关于随机变量均值和方差的灵敏度计算公式,进而根据灵敏度的分析结果,提出多种失效模式下多目标优化的可靠性稳健设计模型。数值算例表明,本文方法可以高效迅速地估计多失效模式下机械构件的可靠性灵敏度。最后还对其进行了可靠性稳健优化设计研究。      

复合材料开孔层板压缩渐进损伤分析

首先,针对纤维增强复合材料开孔层板进行了压缩试验,通过微距数显设备、电镜扫描和X光扫描设备检测了加载过程中的渐进损伤和试验件最终破坏模式,观测了损伤起始和45°与90°铺层间的分层现象. 其次,将复合材料开孔层板失效分为层内失效和层间失效,基于细观损伤力学MMF3理论和界面胶层单元方法建立了开孔压缩损伤跨尺度分析模型.最后,应用该模型对开孔压缩损伤起始、损伤扩展和层板破坏模式进行了预测,获得了纤维和基体损伤起始位置、分层产生位置及扩展过程、最终的分层和压入破坏等计算结果.计算结果与试验结果获得了较好的吻合,表明该计算模型适用于分析复合材料开孔压缩渐进损伤问题.      

基于应变不变量失效理论的复合材料损伤模拟

应变不变量失效理论基于物理失效模式判断纤维和基体的损伤,适于研究纤维与基体的细观相互作用及固化残余应力的影响.介绍了应变不变量失效理论的物理背景,建立了正方形、六边形和钻石型细观代表体积单元模型,给出了宏观应变到细观应变的转换方法,提出了相应的失效模式和损伤演化准则.基于应变不变量失效理论求得了CCF300/5228材料体系的机械应变放大系数和热应变放大系数,对CCF300/5228复合材料开孔层合板的拉伸破坏过程进行了模拟,分析了纤维和基体的失效过程.计算与试验结果取得了较好的一致性,证明了该理论的适用性.     

X射线天文卫星观测需求分析与控制总体设计

对X射线天文卫星观测需求进行了分析,提炼了观测任务对观测模式、源的高精度定位与对准、轨道、热控、测控数传等多项需求与约束;针对X射线观测的多需求、多约束难点,设计了集巡天观测、定点观测与小天区扫描观测于一体的观测模式,解决了一颗卫星同时实现全天扫描、银道面深度扫描、重要惯性区域扫描、重要及机遇目标深度观测以及伽马暴全天监测的多种观测需求的难题,该技术已在我国硬X射线调制望远镜卫星上得到应用.     

Ionospheric electron heating by a rocket borne electron accelerator

A “mother-daughter” rocket code-named “Electron 2” was launched from And?ya, Northern Norway in November, 1978. The “daughter”, carrying a 10 keV electron accelerator, was separated from the “mother” payload with a speed of 0.4 m/s. A series of plasma diagnostic instruments were included on the “mother” to study effects produced by the interaction between the electron beam and the ionospheric plasma. Results obtained by two different plasma probes are presented. It was found that pronounced changes in the ambient electron population took place in regions penetrated by the electron beam. Estimates of the dimensions of the disturbed region are presented.     

Experiments with injection of powerful plasma jet into the ionosphere

This paper describes two rocket experiments “Aelita” with high power lithium plasma injection. The results of onboard magnetometer, massspectrometer, photometer, plasma, corpuscular and ground radar measurements are given. Dynamics and structure of plasma formation are discussed.     

On the importance of fluff on the electric behaviour of cosmic grains

A model is created to describe the effects of “fluff” on the potential and electric field on and close to a charged spherical body embedded in a plasma. The consequences are investigated for dust grains biased at positive or negative potentials, but large enough for electron or ion field emission to be active, especially grains in magnetospheric plasmas. Electron emission reduces the floating potential, whereas ion emission destroys the fluff or even the grain itself. Effects of encounters are discussed. The model also characterizes the levitation of small solid particles from larger bodies.     

Energy spectra of high energy electrons and hard X-rays as observed onboard the space probe Venera 11 during the solar flare event of April 13 1979

The event was observed onboard the space probe Venera 11 at a heliolongitude close to 57°. Electron spectra in the energy range from 60 to 2100 keV are determined and compared with X ray spectra. As a result it was found that conditions of the “thin target” model were realized in the April 13, 1979 flare. Estimates of the total number of accelerated electrons and the energy of the flare are presented.     

弱测量数据下的关机时间估计及其精度分析

通过分析关机后无助推的飞行器落点预报的问题,可以知道落点的精度取决于关机点处的轨道参数,即时间、速度和位置的准确程度,其中关机时间是影响落点精度的主要因素。文章主要研究了在测量数据不完整或缺少的情况下对关机时间的估计问题,并对其精度作了分析,并给出了仿真结果。     

A Cosmic Microscope to Probe the Universe from Present to Cosmic Dawn:Dual-element Lowfrequency Space VLBI Observatory

A space-based Very Long Baseline Interferometry (VLBI) program, named as the Cosmic Microscope, is proposed to involve dual VLBI telescopes in the space working together with giant ground-based telescopes (e.g., Square Kilometre Array, FAST, Arecibo) to image the low radio frequency Universe with the purpose of unraveling the compact structure of cosmic constituents including supermassive black holes and binaries, pulsars, astronomical masers and the underlying source, and exoplanets amongst others. The operational frequency bands are 30, 74, 330 and 1670 MHz, supporting broad science areas. The mission plans to launch two 30-m-diameter radio telescopes into 2 000 km×90 000 km elliptical orbits. The two telescopes can work in flexibly diverse modes. (i) Space-ground VLBI. The maximum space-ground baseline length is about 100 000 km; it provides a high-dynamic-range imaging capacity with unprecedented high resolutions at low frequencies (0.3 mas at 1.67 GHz and 20 mas at 30 MHz) enabling studies of exoplanets and supermassive black hole binaries (which emit nanoHz gravitational waves). (ii) Space-space single-baseline VLBI. This unique baseline enables the detection of flaring hydroxyl masers, and more precise position measurement of pulsars and radio transients at mas level. (iii) Single dish mode, where each telescope can be used to monitor transient bursts and rapidly trigger follow-up VLBI observations. The large space telescope will also contribute in measuring and constraining the total angular power spectrum from the Epoch of Reionization. In short, the Cosmic Microscope offers astronomers the opportunity to conduct novel, frontier science.      

航空电源系统FMEA自动化技术研究

以飞机电源系统为例提出了一种在系统设计阶段，利用系统动态性能仿真模型自动进行定量故障模式影响分析的方法。该方法将系统中各个元器件可能的故障模式计入系统的动态模型中，并进行系统仿真，再将系统故障状态下的仿真结果与其正常状态下的仿真结果进行比较，以量化判定每种故障影响的严重程度，从而实现故障模式影响分析的自动化。     

用面向对象技术实现相关分离的双语言描述

介绍了一种新的形式化描述思想,即"相关分离"的思想,并分析了基于此思想的双语言方法,与传统的单一语言的描述技术相比,"相关分离"的思想和双语言方法更适合于分布式多媒体的描述.结合对面向对象技术在分布式多媒体的形式化描述中应用的方法分析,本文提出了一种以LOTOS/QTL或Esterel/QL为基础,融合面向对象技术的形式化描述方案,该方案可用于建立分布式多媒体系统的时间模型和同步模型.     

Where will efficient energy release occur in 3-D magnetic configurations?

The energy needed to power flares is thought to be stored in the coronal magnetic field. However, the energy release is efficient only at very small scales. Magnetic configurations with a complex topology, i.e. with separatrices, are the most obvious configurations where current sheets can form, and then, reconnection can efficiently occur. This has been confirmed for several flares computing the coronal field and comparing the locations of the flare loops and ribbons to the deduced 3-D magnetic topology. However, this view is too restrictive taking into account the variety of observed solar flaring configurations. Indeed, “Quasi-Separatrix Layers” (QSLs), which are regions where there is a drastic change in field-line linkage, generalize the definition of separatrices. They let us understand where reconnection occurs in a broader variety of flares than separatrices do. The strongest electric field and current are generated at, or close to where the QSLs are thinnest. This defines the region where particle acceleration can efficiently occur. A new feature of 3-D reconnection is the natural presence of fast field-line slippage along the QSLs, a process called “slip-running reconnection”. This is a plausible origin for the motions of the X-ray sources along flare ribbons.     

The TUS space fluorescence detector for study of UHECR and other phenomena of variable fluorescence light in the atmosphere

The Tracking Ultraviolet Set Up (TUS) instrument has been designed to observe from space the fluorescence light in the atmosphere when Extensive Air Shower (EAS) or other phenomena such as meteors or dust grains traverse it. The TUS design concepts will allow us to construct the next generation of fluorescence detectors with increasing light collection power and higher resolution. The KLYPVE instrument with collection power 5 times larger of the TUS will be the next space detector. Light collection is obtained with the help of segmented “low frequency Fresnel type” mirrors. Photo receiver retina in the focal consists of modules of PM tubes. For stable performance in conditions of variable light noise and variable temperature the tube type with a multi-alcali cathode was chosen. Voltage supplies for PMT in one module were designed for keeping the performance of photo receiver retina uniform when the tube gain change. From every tube the signal amplitude is recorded in time bins of 400 ns. The digital data are kept and analyzed in the module FPGA connected to the central FPGA controlling all data. The RAM memory is large, capable to record events with different duration of the light signal (up to several seconds). The preliminary event data are analyzed in the triggering system of the central FPGA. The trigger criteria have several options for events of different origin (different pixel signal duration). The trigger integration time is controlled from the space mission center. The performances of the detector were simulated and zenith angle dependent trigger efficiencies were calculated. The TUS detector will be efficient in recording “horizontal” EAS (zenith angles more than 60°), developed to their maximum above the cloud cover. The EAS Cherenkov light, back scattered from the cloud cover, will be recorded and will improve data on the EAS direction and position of maximum. For better accuracy in physical parameters of the events and for the experimental check of this accuracy the performance of two TUS detectors at the space platform was recommended. The accommodation of 2 TUS detectors at space platform of the “RESURS O” type was tried and approved. The TUS prototypes are being tested in the Mexican mountains. The photo receiver of two PM tubes with the TUS electronics on-board of the MSU Tatiana satellite is measuring the atmosphere light background.