探测快中子的新技术（二）

（上接1997年第17卷第1期第35页）2·4中子的直接探测SIOb。dri。n「13］报道了中子直接探测的原理及可能的方法。在介质中，中子的速度超过光速时，由于中子具有磁偶极矩p—一1．91p。，象带电粒子产生cherenkov效应一样，可以发远紫外光，探测这些光可实现中子的直接探测。光的频谱与户平方正比，与折射指数n有关。可测最小中子能量与折射指数n有关，n越大，E越小，用GaAs最／J’E为15MeV。直接探测的优点是效率高、不需另外的零时刻即可做飞行时间测量等。·2．5多元件阵列快中子探测器和极化仪在中高能和重离子核物理中，中子能量可…     

电子加速器在大型工业CT中的应用研究

以大型工业CT 检测系统中的电子加速器 X 射线源为研究对象,分析了驻波电子加速器在大型工业 CT 应用中遇到的能量选择、张角的大小、能量空间分布问题;并从理论上分析研究了高能 X 射线在探测器之间的相互窜扰的影响,给出了高能 X 射线窜扰的校正方法。     

民航机组人员所受宇宙辐射的剂量水平,危害及防护

宇宙辐射来自银河系,主要由具极高能量的氦核组成,一个粒子能量10~(20)eV(电子伏特)换成机械能就能把一本书上举1m。初始辐射与地球大气层作用生成次级辐射,由电离成分(μ介子、快速点子和γ线等)和中子组     

电子能量损失谱及其在复合材料界面研究中的应用

在介绍电子能量损失谱基本原理的基础上，阐述了电子能量损失谱高能损失区在复合材料界面研究中的应用，最后，对电子能量损失谱和Ｘ射线能谱分析进行了比较。     

Wolter-Ⅰ型X射线脉冲星探测器的空间环境本底分析

X射线脉冲星导航具有自主性强、抗干扰、安全性高等特点。针对X射线脉冲星辐射信号的探测与识别介绍了一款Wolter-Ⅰ型X射线脉冲星探测器。为评估探测器的性能、提升灵敏度，对该Wolter-Ⅰ型X射线脉冲星探测器开展了蒙特卡罗(MC)模拟研究。首先基于空间环境信息系统(SPENVIS)平台给出运行轨道中不同种类带电粒子的分布与能谱特征；然后采用GEANT4软件构建了Wolter-Ⅰ型X射线脉冲星探测器的质量模型，模拟了探测器对电子、质子及氦等带电粒子的响应；最后以遮光膜参数优化为例说明探测器优化方式，并给出优化后探测器在700 km地球圆轨道上的空间环境本底。结果表明优化后探测器的空间环境本底为30.68 cts·s^-1。     

空间高能宇宙辐射探测设施HERD

空间高能宇宙辐射探测设施HERD主要科学目标为暗物质的搜寻、原初宇宙射线各成分能谱的精细测量以及伽玛射线巡天观测。HERD主要由一个五面灵敏的三维成像量能器和除底面之外全包络的硅径迹探测器构成。量能器包括约1万块硅酸钇镥(LYSO)晶体,实现入射粒子能量测量以及入射粒子种类的鉴别;硅径迹探测器由x-y方向正交排列的硅微条探测器组成,实现入射粒子方向、径迹的测量并测量入射粒子电荷。HERD的主要设计指标为:100Ge V以上能区的电子和伽玛射线探测能量分辨为1%,10 Ge V到1 Pe V能区的质子探测能量分辨为20%;200 Ge V时电子和弥散伽玛射线的有效几何因子大于3 m2sr,100 Te V时宇宙线核素的有效几何因子大于2 m2sr。量能器晶体创新性地采用波长位移光纤+ICCD读出方案,提高了在轨运行工程可行性。     

ACTIS 1305/120-1220轮胎X-射线自动检测系统

用途主要用于汽车子午线轮胎内部帘线与钢丝带束层排市状况的检测；轮胎内部气孔、缝隙。裂纹等缺陷的检测；轮胎胎留部位、帘布反包高度、三角胶与胎圈粘合情况的检测等。技术指标和参数·被检测轮胎的参数轮胎尺寸最小最大轮胎外径500mm1126mm胎面宽度130mm320mm胎圈直径12″20″轮胎重量57kg检测能力本系统一分钟可检测两条轮胎，并能适应三班制连续工作。各部分的定位精度探测器运动机构的定位精度：Y向±1．5mmX向±5．0mmX-射线测试转台扩毂精度；±2.0mmX-射线管伸缩运动的定位精度；±2.0mm系统定位精度±3．0mm轮胎旋转的转…     

EXAFS-Ⅰ型扩展X射线吸收谱仪电气工作原理

本文介绍用于对物质结构进行精细分析的EXAFS-Ⅰ型扩展X射线吸收谱仪的电气工作原理、仪器性能和试验结果。     

单晶涡轮叶片高能束修复研究进展

单晶涡轮叶片高能束增材再制造是修复磨损、烧蚀和裂纹等损伤缺陷的主要方式，是航空发动机热端部件特种加工领域最具挑战性的工作之一，其中蕴含的外延生长组织接续与调控机制、内部冶金缺陷控制等科学问题和关键工艺尚未完全突破。梳理了熔焊熔池内凝固组织定向生长的理论发展，基于已有的枝晶异质形核和异向生长理论，构建了单晶高能束修复的基础原理框架；详细分析了“修复工艺-熔池特性-凝固组织”之间的内在关联，提出了保持单晶连续稳定生长的工艺调控准则和熔池监控方法；总结了修复区γ′相等微观组织以及热裂纹、气孔等冶金缺陷的演化规律和调控手段，凝练了单晶修复面临的主要挑战。此外，介绍了航空发动机热端部件再制造领域相关的国外重大研究计划，并对今后研究方向和发展趋势进行总结和展望。     

核輻照对合金磁性能的影响

对Fe—Si、Fe—Ni、Fe—Co及Fe—Ni—Co系合金在电子流、质子流、快中子流和γ射线中磁性能的变化进行了测试。测试结果表明,除经横向热磁处理的1J66及1J67h合金外,其它合金的磁性能没有明显的变化。     

The Cosmic Ray Nucleonic Component: The Invention and Scientific Uses of the Neutron Monitor – (Keynote Lecture)

The invention of the neutron monitor pile for the study of cosmic-ray intensity-time and energy changes began with the discovery in 1948 that the nucleonic component cascade in the atmosphere had a huge geomagnetic latitude dependence. For example, between 0° and 60° this dependence was a ∼ 200–400% effect – depending on altitude – thus opening the opportunity to measure the intensity changes in the arriving cosmic-ray nuclei down to ∼1–2 GeV nucl⁻¹ for the first time. In these measurements the fast (high energy) neutron intensity was shown to be a surrogate for the nuclear cascade intensity in the atmosphere. The development of the neutron monitor in 1948–1951 and the first geomagnetic latitude network will be discussed. Among its early applications were: (1) to prove that there exists interplanetary solar modulation of galactic cosmic-rays (1952), and; (2) to provide the evidence for a dynamical heliosphere (1956). With the world-wide distribution of neutron monitor stations that are presently operating (∼ 50) many novel investigations are still to be carried out, especially in collaborations with spacecraft experiments. This revised version was published online in August 2006 with corrections to the Cover Date.     

用大面积源检定核应急机载/车载伽玛能谱仪

人工核素大面积源标准是核工业航测遥感中心等单位经过十余年研究建立的新型计量保障标准,使用该标准,可对监测核应急伽玛辐射环境的机载/车载伽玛能谱仪进行检定.使用大面积源标准检定,可以有效地弥补因机载/车载伽玛能谱仪系统的角响应影响因素复杂而难于模拟计算的缺陷,为监测核应急伽玛辐射环境的机载/车载伽玛能谱仪提供了量值传递的保障.本文介绍了大面积源检定的原理和技术方法.     

An Overview of the Instrument Suite for the Deep Impact Mission

A suite of three optical instruments has been developed to observe Comet 9P/Tempel 1, the impact of a dedicated impactor spacecraft, and the resulting crater formation for the Deep Impact mission. The high-resolution instrument (HRI) consists of an f/35 telescope with 10.5 m focal length, and a combined filtered CCD camera and IR spectrometer. The medium-resolution instrument (MRI) consists of an f/17.5 telescope with a 2.1 m focal length feeding a filtered CCD camera. The HRI and MRI are mounted on an instrument platform on the flyby spacecraft, along with the spacecraft star trackers and inertial reference unit. The third instrument is a simple unfiltered CCD camera with the same telescope as MRI, mounted within the impactor spacecraft. All three instruments use a Fairchild split-frame-transfer CCD with 1,024× 1,024 active pixels. The IR spectrometer is a two-prism (CaF₂ and ZnSe) imaging spectrometer imaged on a Rockwell HAWAII-1R HgCdTe MWIR array. The CCDs and IR FPA are read out and digitized to 14 bits by a set of dedicated instrument electronics, one set per instrument. Each electronics box is controlled by a radiation-hard TSC695F microprocessor. Software running on the microprocessor executes imaging commands from a sequence engine on the spacecraft. Commands and telemetry are transmitted via a MIL-STD-1553 interface, while image data are transmitted to the spacecraft via a low-voltage differential signaling (LVDS) interface standard. The instruments are used as the science instruments and are used for the optical navigation of both spacecraft. This paper presents an overview of the instrument suite designs, functionality, calibration and operational considerations.     

The quiescent spectrum of 2S1636-536

During the EXOSAT observation of 2S1636-536 in July 1983 the quiescent flux was observed to brighten from 1.7×10 ^-9 ergs/cm. ² /sec to 2.6×10^-9 ergs/cm. ² /sec, this increase being accompanied by a decrease in effective temperature. Further analysis of the spectrum reveals that the best fit is a power law with an index which increases from -1.75 to-2.1 while the source brightens; there is some evidence for an upper cut off. This spectrum is interpreted as the result of soft photons from the neutron star surface which are Comptonised in a hot plasma cloud surrounding the neutron star (neutron star corona). The increasing spectral index is seen as the result of Compton cooling of the corona as the output of quiescent flux rises in response to an increasing accretion rate.     

Neutron Monitor Design Improvements

The original design by J. A. Simpson of the neutron monitor enabled continuous monitoring of the primary cosmic-ray flux by ground-based recordings of the nucleonic component with only a rather simple correction for atmospheric effects. Simpson (1957) extended the original pile to the 12 counter IGY neutron monitor which was deployed in a world wide network during the International Geophysical Year 1957/8. The desirability for monitors with higher counting rates became evident soon afterwards. Subsequently the NM64 super neutron monitor was designed by H. Carmichael for deployment in time for the International Quiet Sun Year 1964. Using unusually large ¹⁰BF₃ proportional counters made at Chalk River, Hatton and Carmichael (1964) studied comprehensively the experimental design of the NM64. Consequently the efficiency of neutron counters to record evaporation neutrons produced in the lead of a monitor increased from 1.9% for the IGY to 5.7% for the NM64, an increase of 3.3 times the counting rate per unit area of lead producer. During the years much attention was given to the neutron multiplicity spectrum in neutron monitors. This spectrum is related to the energy spectrum of the nucleonic component incident on the neutron monitor, but is only weakly dependent on the spectrum of galactic cosmic rays at the top of the atmosphere. Contrary to galactic cosmic rays, solar flare protons and neutrons are observed predominantly as single counts per interaction, in multiplicity 1, because of the softness of solar flare particle energy spectra. Neutron monitors have also been specially designed to record solar neutrons with increased sensitivity. Newly developed ³He counters with a largely reduced thermal neutron absorption mean free path should lead to improved efficiency in recording primary cosmic radiation. Design criteria are discussed. This revised version was published online in August 2006 with corrections to the Cover Date.     

ZrC 粉体制备的研究进展

ZrC作为一种先进的高温结构陶瓷材料,在航空航天、清洁能源(第四代核技术)等领域具有广泛的应用。本文主要综述了ZrC粉体的制备技术,主要有直接合成法、机械合金化法、自蔓延高温合成法、碳热还原法、溶胶-凝胶法、液相前驱体法、激光气相反应法和高频等离子体法等,详细分析了各制备技术的特点。     

The Mars Odyssey Gamma-Ray Spectrometer Instrument Suite

The Mars Odyssey Gamma-Ray Spectrometer is a suite of three different instruments, a gamma subsystem (GS), a neutron spectrometer, and a high-energy neutron detector, working together to collect data that will permit the mapping of elemental concentrations on the surface of Mars. The instruments are complimentary in that the neutron instruments have greater sensitivity to low amounts of hydrogen, but their signals saturate as the hydrogen content gets high. The hydrogen signal in the GS, on the other hand, does not saturate at high hydrogen contents and is sensitive to small differences in hydrogen content even when hydrogen is very abundant. The hydrogen signal in the neutron instruments and the GS have a different dependence on depth, and thus by combining both data sets we can infer not only the amount of hydrogen, but constrain its distribution with depth. In addition to hydrogen, the GS determines the abundances of several other elements. The instruments, the basis of the technique, and the data processing requirements are described as are some expected applications of the data to scientific problems.     

Neutron measurements in space

The experimental measurements of the neutron flux and energy spectrum in space since 1964 are reviewed and related to the theoretical predictions. A discussion of the neutron sources is presented. The difficulties associated with neutron measurements of both the atmospheric neutron leakage flux and solar neutrons are included. Particular emphasis is placed upon the neutron leakage flux and energy measurements at energies greater than about 1 MeV. The possibilities of CRAND as a source for the energetic trapped protons are discussed in light of recent measurements of the 10–100 MeV neutron flux. The current status of the solar neutron flux observations is also presented.The primary purposes of neutron measurements in space have been to determine the neutron leakage flux from the atmosphere of the Earth and the solar neutron flux. As a consequence of the inefficient methods for neutron detection and the difficulties of conducting the measurements in the presence of the galactic and solar cosmic-ray backgrounds, the experimental results are very conflicting. It is the purpose of this review to interpret and discuss recent neutron measurements. In order to understand these results the theoretical predictions of the neutron fluxes and energy spectra from possible neutron sources will be briefly presented. Since comparisons of the different neutron measurements depend critically upon the experimental techniques, we will briefly discuss neutron detection methods applicable to space measurements. The emphasis will be upon measurements since 1964 made outside the Earth's atmosphere, but considerable reference will be made to high energy neutron experiments conducted within the Earth's atmosphere at < 10g cm^-2 altitude. A review of earlier neutron measurements of terrestrial and solar neutrons has been made by Haymes (1965).     

超声速逆向喷流的减阻与降热

利用流动控制技术改变流场结构的方法,对逆向冷喷流将激波推离物体表面以达到减阻减热的效果,进行了数值模拟计算。通过计算给出了钝头体在超声速流场中有无逆向喷流的压力场和温度场的比较,结果表明,逆向喷流对钝头体表面的减阻和减热起到了明显的作用。     

Global avionics in the future

The following topics are discussed: new batteries for old airplanes; new charge controls for lengthening battery life; fast methods for batteries charging; AC conductance measurement based battery testing; pulse power; bipolar lead-acid batteries vs supercapacitors; Ni electrode cells for spacecraft; worn-out battery disposal; recycling technology; vehicle batteries cost; high energy content batteries; and energy storage for electric utilities