放射性勘查计量的发展及关键技术

放射性勘查计量从1958年开始简易点源标定,到1978年开始建立与天然辐射场2盯空间辐射近似的实物模型标准,经历了约20年的仪器检查性测试计量和30余年的统一标准计量的发展历程,先后共研建了12项计量标准和1项模拟试验装置,其中4项标准已获得了国家专项计量授权。从中掌握了多项关键技术,形成了独特的放射性勘查计量保障体系,计量保障涵盖了放射性区域调查、局部详查、钻探等整个勘查过程,在为国家放射性勘查提供计量保障的同时,还为核应急、核设施退役等伽玛辐射环境航空监测提供了计量保障。     

机载反辐射武器作战使用研究

机载反辐射武器是对付地面防空雷达的有效手段。综述了机载反辐射武器的工作原理、技术特点及作战使用。     

机载时间敏感组网分析综述

时间敏感网络“准时、准确”的调度与传输机制可以有效地提升工业自动化系统、车载综合电子系统中信息交互的确定性，潜在的也成为了机载系统高确定性组网的候选方案之一，但如何将其多种时间敏感整形和调度机制与机载组网环境和需求进行匹配，是当下首要解决的问题。在对现阶段的时间敏感网络的标准进行总结的基础上，详细分析了机载组网的需求，并从时间敏感网络调度与优化、保证时延边界分析两方面总结了当下时间敏感网络相关研究的最新进展，以及与机载组网环境相结合的考虑，进一步针对机载组网的典型需求，从协议剪裁、体系管理、模型工程、可靠安全、无线混传等方面详细讨论了时间敏感网络技术在机载环境应用所面临的挑战和关键技术。     

某型机载雷达告警系统标定方法与环境构建

机载雷达告警系统在使用过程中会出现告警误差,需要定期对其性能参数进行标定校验。本文介绍了机载告警系统常见性能参数,研究给出了信号辐射法和直接馈入法的标定条件、环境构建方式、标定所需器材、标定流程,对科学指导机载告警雷达系统的标定具有重要意义。     

机载适航标准DO-178B/C软件开发过程研究

介绍了DO-178B/C标准的发展历程,结合对DO-178B/C标准机载软件生命周期过程的研究,分析了机载软件开发过程需求、设计、编码和集成子过程的关系及输入输出数据,在分析机载软件需求、设计、编码及集成子过程的目标、活动和转换准则的基础上,给出了各子过程的过程模型.展望了DO-178B/C标准的未来研究方向.     

S-92A直升机上的状态与使用监测系统

详细介绍了S-92A直升机状态与使用监测系统机载部分:综合机械诊断式状态与使用监测系统、轴承监测单元、数据传递单元、维护数据库处理器的有关情况.总结了S-92A直升机状态与使用监测系统的新特点.     

1750A标准机载计算机设计与研制

1750A 标准机载计算机是在军用机载恶劣环境下使用的标准化、模块化的微机系统,有1ATR 机型和1/2ATR 机型。主处理器采用 FAIRCHILD F8450芯片,主频时钟为20HHZ,采用标准化的单(?)模块式结构,运行速度大于0.(?)MIPS,(?)机1988年底通过航空工业部科技局主持的阶段评审。     

静电电荷衰减试验仪检定装置研究

为给电荷衰减时间测试仪器提供溯源,研制了一套电荷衰减试验仪检定装置.该装置主要由双指数形标准衰减电压源、标准脉冲分压器和计算机数据采集处理系统等三个重要部分组成,数据采集处理系统采用虚拟仪器软件Lab Windows/CVI编制,该装置的扩展不确定度为0.66%.     

燃油流量标准装置测控系统开发

利用PLC、PC和单片机开发的燃油流量标准装置测控系统,最大限度地挖掘了标准装置检定校准燃油流量传感器的能力,保障了航空发动机试验数据准确可靠,在实际使用中取得了很好的效果。     

一种窄带辐射温度计智能标定及检定系统

文章描述了由串行电可改写擦除存储器（ＥＰＲＯＭ）、ＲＳ－２３２通讯口和个人计算机（ＰＣ）组成的窄带辐射温度计标定检定系统。系统除了能够在标定过程中自动完成仪器的标定，给出听输出误差分布、提高仪器的速度以外，在检定时还可以通过修改检定参数很容易地修正仪器的各种源移量，使被检测仪器无需作入动或调整即可重新使用。     

Compton Polarimetry in Gamma-Ray Astronomy

The analysis of compact astronomical objects has generally dealt with the physical properties of the source within a two-parameter space, which is defined by the spectral characteristics and time variability. This approach often leads to the situation whereby two or more very different models can explain the observations successfully. Polarimetric observations have the diagnostic potential to discriminate between the different compact source models and can offer a unique insight into the geometrical nature of the emission zones. To date, however, no polarization observation in the gamma-ray energy domain has been successfully performed, due to the difficulties in making polarimetric measurements in this high-energy region of the spectrum. In this paper the polarized gamma-ray emission mechanisms are reviewed with the emphasis on their detectable characteristics. Potential astronomical sites in which these emission mechanisms may be at work are discussed. Observational results obtained in other wavebands and theoretical predications made for some of the most likely astronomical sources of polarization are reviewed. Compton polarimetry has long been used in the field of nuclear gamma-ray spectroscopy in the laboratory. The operational principle behind all generations of nuclear gamma-ray polarimeters has been to measure the asymmetry in the azimuthal distribution of the scattered photons. However none of the polarimeters designed for laboratory experiments will be sensitive enough to observe even the strongest astronomical source. In the past few years there have been a number of innovative developments aimed at the construction of astronomical gamma-ray polarimeters, either as dedicated experiments or in missions with polarimetric capability. The designs of all the polarimeters are based on either discrete or continuous position sensitive detector planes. In this paper the data analysis techniques associated with this type of polarimeter are discussed as well as methods of removing some of the systematic effects introduced by a non-ideal detector response function and observation conditions. Laboratory tests of these new polarimetric techniques are reviewed. They demonstrate the feasibility of building a suitably sensitive astronomical gamma-ray polarimeter. Optimization of the design of pixellated detector array based polarimeters is also addressed. The INTEGRAL mission, which is to be launched by ESA in the year 2001, is the most likely telescope to perform the first successful gamma-ray polarization observation. The polarimetric characteristics of the two main instruments on board INTEGRAL are evaluated and their sensitivities to a wide range of potentially polarized gamma-ray sources are estimated.     

Determining the Absolute Abundances of Natural Radioactive Elements on the Lunar Surface by the Kaguya Gamma-ray Spectrometer

The Kaguya gamma-ray spectrometer (KGRS) has great potential to precisely determine the absolute abundances of natural radioactive elements K, Th and U on the lunar surface because of its excellent spectroscopic performance. In order to achieve the best performance of the KGRS, it is important to know the spatial response function (SRF) that describes the directional sensitivity of the KGRS. The SRF is derived by a series of Monte Carlo simulations of gamma-ray transport in the sensor of the KGRS using the full-fledged simulation model of the KGRS, and is studied in detail. In this paper, the method for deriving absolute abundance of natural radioactive elements based on the SRF is described for the analysis of KGRS data, which is also applicable to any gamma-ray remote sensings. In the preliminary analysis of KGRS data, we determined the absolute abundances of K and Th on the lunar surface without using any previous knowledge of chemical information gained from Apollo samples, lunar meteorites and/or previous lunar remote sensings. The results are compared with the previous measurements and the difference and the correspondence are discussed. Future detailed analysis of KGRS data will provide new and more precise maps of K, Th and U on the lunar surface.     

浮子流量计检定装置的研制

介绍了一种型号为LB311非水液体浮子流量计检定装置,该装置基于标准表法,采用一大一小离心泵来提供稳流源,用涡轮流量计作为标准表来检定浮子流量计,测试流量范围宽;采用三阀调节系统,调节精度高.     

Background in space-borne low-energy γ-ray telescopes

The scope of observational astronomy in the gamma-ray region of the spectrum is vast. The intimate relationship of these energetic photons with their parent particles and fields provides a direct probe of the high-energy physics phenomena which take place throughout the Universe. As an added bonus the gamma-ray domain contains a wealth of diagnostic information within discrete emission lines, which are derived from a variety of processes including nuclear de-excitation, cyclotron emission, and matter-antimatter annihilation. Consequently observational gamma-ray astronomy addresses directly some of the most fundamental problems in both physics and astrophysics. However, low-energy gamma-rays are the most penetrating photons encountered in nature, and, whilst this factor provides a deep probe of cosmic objects, it ensures that gamma-ray telescopes are massive, both in terms of the stopping power required in the detector systems as well as their shields. Furthermore, the intimate relationship of gamma-rays with nuclear de-excitations ensures that the telescope itself becomes a bright source of background noise, a factor which is aggravated by the necessity that gamma-ray telescopes are obliged to operate in regions pervaded by intense particle fluxes. The background noise experienced in gamma-ray telescopes is, therefore, both high and extremely complex in its origin, and due to the high-energy content of individual photons, their numbers which arrive from distant cosmic sources are necessarily low, even for those objects which radiate the bulk of their power at gamma-ray wavelengths. Current gamma-ray telescopes are thus obliged to operate under conditions of intrinsically low signal-to-noise ratio and it is vital that techniques are developed which reduce the background noise level to more acceptable levels, thus improving the sensitivity. To achieve such a goal, a thorough understanding of the sources of background noise is first required before effective measures can be taken for its reduction.In this paper the sources of background noise are reviewed with the aim to obtain a quantitative analysis of individual contributions, as derived from the various classes of irradiative particle fluxes. The estimated contributions from the individual sources are combined in order to evaluate the total background level of a given telescope in a specific radiation environment, which for practical considerations generally relates to the orbit choice and detailed design of the telescope. The published background noise spectra of a number of past missions are compared to the computed values so as to provide an assessment of the validity of the overall calculations. The level of agreement achieved indicates that a good understanding of the sources of background noise exists. Finally some possibilities for the improvement of the sensitivity of future gammaray telescopes, in terms of the reduction of the background noise, are discussed.     

Impacts of solar and auroral storms on power line systems

A sensitive search for pulsars inside a sample of gamma-ray source error boxes has been carried out using the Arecibo and Parkes radiotelescopes. The paper describes the motivation of this search and the characteristics of the experiments used. As a preliminary result, new pulsars have been discovered and some of them are possibly candidates to be the counterparts of the gamma-ray sources.     

Cosmic gamma-ray bursts

The observational characteristics of gamma-ray bursts are reviewed, concerning their spectra as well as their temporal structure and spatial distribution. From this data, it is suggested that the sources belong to a thick halo population (scale height > 3 kpc), and that the mean recurrence time for one source is greater than 5 yr. The implications of these results are discussed, concerning the future experimental perspectives of detection of gamma-ray bursts, and also the constraints on theoretical models.     

Inverse-compton gamma rays from plerions

Young pulsars surrounded by supernova remnants can power synchrotron nebulae through the injection of relativistic particles. Inverse Compton scattering by the high-energy electrons and positrons can produce TeV gamma-ray emission strong enough to be detectable by ground-based telescopes. The Crab nebula is the archetypical example of a gamma-ray plerion and was the first detected TeV source. The observed spectrum is consistent with predictions of synchrotron-self Compton models. This paper will review such models for the Crab and other plerions. Inverse-Compton scattering on other soft photon sources, particularly the 2.7K microwave background, may also be detectable in older remnants.     

The X-ray/Gamma-ray Spectrometer on the Near Earth Asteroid Rendezvous Mission

An X-ray/gamma-ray spectrometer has been developed as part of a rendezvous mission with the near-Earth asteroid, 433 Eros, in an effort to answer fundamental questions about the nature and origin of asteroids and comets. During about 10 months of orbital operations commencing in early 1999, the X-ray/Gamma-ray Spectrometer will develop global maps of the elemental composition of the surface of Eros. The instrument remotely senses characteristic X-ray and gamma-ray emissions to determine composition. Solar excited X-ray fluorescence in the 1 to 10 keV range will be used to measure the surface abundances of Mg, Al, Si, Ca, Ti, and Fe with spatial resolutions down to 2 km. Gamma-ray emissions in the 0.1 to 10 MeV range will be used to measure cosmic-ray excited elements O, Si, Fe, H and naturally radioactive elements K, Th, U to surface depths on the order of 10 cm. The X-ray spectrometer consists of three gas-filled proportional counters with a collimated field of view of 5° and an energy resolution of 850 eV @ 5.9 keV. Two sunward looking X-ray detectors monitor the incident solar flux, one of which is the first flight of a new, miniature solid-state detector which achieves 600 eV resolution @ 5.9 keV. The gamma-ray spectrometer consists of a NaI(Tl) scintillator situated within a Bismuth Germanate (BGO) cup, which provides both active and passive shielding to confine the field of view and eliminate the need for a massive and costly boom. New coincidence techniques enable recovery of single and double escape events in the central detector. The NaI(Tl) and BGO detectors achieve energy resolutions of 8.7% and 14%, respectively @ 0.662 MeV. A data processing unit based on an RTX2010 microprocessor provides the spacecraft interface and produces 256-channel spectra for X-ray detectors and 1024-channel spectra for the raw, coincident, and anti-coincident gamma-ray modes. This paper presents a detailed overview of the X-ray/Gamma-ray Spectrometer and describes the science objectives, measurement objectives, instrument design, and shows some results from early in-flight data.     

Large-scale structure of the Galaxy and high-energy gamma-ray observations

Detailed information on the high-energy gamma-ray emission from our Galaxy has become available through the two dedicated satellite missions SAS-2 and COS-B. The consistency of the two datasets is discussed; while a satisfying general agreement is observed, a few distinct discrepancies point to possible time variations within the compact source component of the total galactic emission. The bulk of emission appears very well correlated to the column density of the total interstellar gas, as traced by radio observations of Hi and CO. The gamma-ray observations exclude the possibility that H₂ dominates in the inner Galaxy, its mass should not exceed the mass existing in the form of Hi. Neither a significant galactocentric gradient of the (high-energy) cosmic-ray flux density is suggested inside the solar circle (outside a decrease is needed), nor a linear coupling between the cosmic rays and the gas is indicated by the gamma-ray data. The systematic variation with longitude of the spectrum of the gamma-ray emission points to an increased flux of cosmic-ray electrons in the 100 MeV to 1 GeV energy range in regions where dense clouds are concentrated. The variation could as well be due to the largely unresolved population of compact gamma-ray objects.     

The Energy Spectra and Anisotropies of Cosmic Rays

The existing paradigm of the origin of Galactic cosmic rays places strong supernovae shocks as the acceleration site for this material. However, although the EGRET gamma-ray telescope has reported evidence for GeV gamma rays from some supernovae, it is still unclear if the signal is produced by locally intense cosmic rays. Although non-thermal X-ray emissions have been detected from supernova remnants and interpreted as synchrotron emission from locally intense electrons at energies up to 100 TeV, the inferred source energy spectral slopes seem much steeper than the electron source spectrum observed through direct measurements. It remains the case that simple energetics provide the most convincing argument that supernovae power the bulk of cosmic rays. Two characteristics which can be used to investigate this issue at high energy are the source energy spectra and the source composition derived from direct measurements.