虚拟仪器在肼类推进剂监测中的应用研究

基于对肼类推进剂监测方法和存在问题的探讨,提出了用虚拟仪器技术解决肼类推进剂监测过程中存在的问题,并介绍了虚拟仪器的概念、结构和特点。虚拟仪器在肼类推进剂监测中具有广泛的应用前景。     

~(201)Hg~+离子贮存式频率标准

本文讨论利用在潘宁离子收集器中贮存~201Hg~+离子实现微波频率(和时间)标准以及光频标性能的潜力与存在的问题。有许多讨论一般都适用于离子贮存式频标。激光致冷、光抽运、以及微波或光时钟跃迁的光检测,可利用在194.2nm6P~2P_(1/2)←6~2S_(1/2)跃迁的窄带幅射,而有选择地将基态超精细能级与适当的微波幅射加以混频来完成。特别适用于采用潘宁(冷阴极)离子收集器的一阶独立场微波时钟跃迁是在1.534T 磁场的25.9GHz(F,M_F)=(2,1)←→(1,1)超精细跃迁。在563nm(毫微米)的双量子无多普勒5d~96S~(22)D_(5/2)←→5d~(10)6S~2S_(1/2)迁可能是光频标所要选用的。两种频标的绝对准确度具有达到好于1×10~(-15)而频率稳定度低于10~(-16)的潜力。     

气相色谱法定量分析氧气中气体杂质方法研究

为寻找一种能够有效检测氧气中微量气体杂质的方法,采用配有氢火焰离子化检测器的气相色谱仪分析氧气中的微量气体杂质,研究了分析氧气中CO、CO₂及C₂H₂等气体杂质的操作参数,确定了氧气中微量气体杂质的分析方法,验证了该方法的可行性,该分析方法各组份分离效果良好,各种杂质组份定量精确度较高。     

声表面波气体检测器

本文介绍一种利用声表面波的新型气体检测器的试验结果。声表面波(SAW)压电气体检测器由制作在一块压电衬底上的SAW双延迟线组成,每一延迟线都接有一振荡器。在一根延迟线振荡器的传播路径上涂以选择性吸收薄膜,而在另一传播路径上则不涂复而用作稳定参考。由吸附在涂有薄膜的延迟线上的气体所引起的质量负载或应力效应造成的相位延迟变化,导致相对于参考振荡器的频率偏移。这种频率偏移是与气体浓度成比例的。由于SAW能集中在薄膜附近,故检测器的灵敏度很高。另外,只要给SAW压电气体检测器涂以相应的选择性薄膜,就可以检测任何气体。为了证明这一点,现已制成一个利用三乙醇胺薄膜测量空气中二氧化硫(SO_2)的检测器,并且已经证明能够检测出浓度为10×10~(-9)的二氧化硫。对灵敏度、线性、再现性、选择性和可靠性的研究,发现在大多数情况下比其它类型的气体检测器优越。本文讨论器件性能(例如选择性和随时间的稳定性)的主要缺点,以及改善的可能方法和进一步研究的方向。     

我国走向“碳索”新征程 实现全球温室气体排放监测——解读我国首台干涉型高光谱温室气体遥感器

正2017年11月15日,随风云-3D卫星顺利入轨的我国首台干涉型温室气体观测遥感器——"高光谱温室气体监测仪",将为全球温室气体排放监测、温室气体与气候变化关系等问题的研究提供强有力的数据支持,为建设美丽中国,为人民创造良好的生产生活环境,为全球生态安全作出贡献。该遥感器由中国空间技术研究院北京空间机电研究所历时6年时间研制而成,采用时间调制型干涉分光的技术途径,具有超高光谱分辨率、宽光谱覆盖     

发射箱气密监测方法

通过对导弹贮运发射箱在各种使用环境下的气密性分析 ,建立了发射箱可靠贮存数学模型。根据模型设计了一种通用型内环境气密监测仪 ,对发射箱在贮存、运输状态下的密封性进行动态监测 ,能准确地预测发射箱对导弹的有效贮存期 ,保证导弹的贮存可靠性     

双模式离子液体推进剂的分解特性与热试车实验研究

硝酸羟胺(HAN)/1 乙基 3 甲基咪唑硫酸乙酯(［Emim］［EtSO4］)混合离子液体推进剂具有绿色无毒、高性能、易电离的特点，既可以应用于化学推进模式，又可以应用于电推进模式，是肼类推进剂的一种理想的替代品.利用热重分析 差示扫描量热法(TGA DSC)研究了HAN/［Emim］［EtSO4］离子液体推进剂的热分解和催化分解过程.研究了其在升温速率为5 K/min~15 K/min时，热分解和催化分解情况下的失重过程和放热过程.失重结果表明，该离子液体推进剂分解过程中，放热曲线表明，分解过程存在两个显著的放热过程使用催化剂可以显著地降低推进剂的分解温度和残余质量.最后，研制了推力为200 mN的模型发动机，热试车结果表明，HAN/［Emim］［EtSO4］离子液体推进剂可以在催化点火条件下实现稳定启动，在空间推进领域具有良好应用前景.     

离子推进器对卫星姿态控制系统的干扰

本文针对离子推进器用于地球同步轨道卫星作南北位置保持的几种实用安装布置方案,分析讨论了由于离子推进器推力矢量的角误差、实际推力与名义推力之差、以及卫星质心移动离开它的名义位置所产生的干扰力矩、对应的角冲量及为补偿这些干扰力矩姿态控制系统肼推进器额外需消耗的肼燃料量;推导了在飞行任务期间估算这些量的计算公式. 从分析和计算实例的结果讨论中,还得到一些有益的结论.     

惰性气体整体保护焊接室内气体压力变化分析

针对空间飞行器越来越广泛地使用钛合金材料及材料在传统焊接加工中存在的问题,研制了惰性气体整体保护焊接设备。保护的可靠性与焊接室内的惰性气体纯度密切相关,当利用提高焊接室内的压力这一经济有效的方法来维持焊接室内的气体纯度时,压力的变化则成为我们关心的焦点。分析了惰性气体整体保护焊接工作室中气体压力在焊接操作中的变化情况;讨论了焊接操作带来的对焊接室内气体压力的影响;指出为了在各种情况下使焊接工作室内保护环境免遭破坏必须采用的措施。     

中国碳卫星究竟有多牛?

<正>中国首颗全球二氧化碳监测科学实验卫星(简称"碳卫星")经平台测试、载荷加热排污等一系列工作后,其有效载荷于1月12日成功开机,13日转入在轨观测任务模式并获取首批观测数据。此次获得的数据是通过高光谱二氧化碳监测仪获取,并经过地面处理生成的第一组大气氧气和二氧化碳吸收光谱图,是我国从太空获取的第一组大气氧气和二氧化碳吸收高分辨率光谱图。首批观测数据的成功获     

FY-2C卫星太阳X射线探测器性能定标

通过具体的实验对FY-2C太阳X射线探测器进行了详细的定标.太阳X射线探测器的传感器采用充Ar气的正比计数器.主要探测能量大于4 KeV的太阳X射线流量.在坪特性、效率、正比性、能道划分、能量分辨率和时间分辨率等6个方面详细介绍了定标的方法及结果.定标结果表明,FY-2C卫星的太阳X射线探测器在各个方面都具有很好的性能.最后对FY-2C的在轨探测数据与GOES卫星进行了比较.GOES卫星的太阳X射线传感器采用电离室.FY-2C的探测结果与GOES的探测结果非常吻合.结果表明,FY-2C太阳X射线探测器可以很好地监测太阳X射线的流量变化,为空间环境监测提供有效的服务.      

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.     

First calibration measurements with the dust impact detector DIDSY-IPM

The IPM detector consists of two separate impact ionization detectors, one of them covered by a 2.5 μm thick plastic film and a piezoelectric sensor mounted to the back of the joint impact plate. First impact tests, with iron projectiles in the mass range 10^?15 to 10^?9 g and in the speed range 1 km/s to 70 km/s, were performed with the calibration (FS) and the flight (F) model of this detector. The charge yield at 69 km/s impact speed (flyby speed of GIOTTO) has been extrapolated from the data and amounts to 400 Coulombs per gram. This corresponds to a preliminary sensitivity threshold for the impact ionization detector of about 6×10^?17 g. The penetration limit introduced by the plastic film is about 10^?14 g for iron particles. Only the biggest particles used for the test produced signals at the piezoelectric sensor. If one assumes an energy dependence of the piozoelectric signal, a preliminary sensitivity threshold of about 10^?13 g at 69 km/s can be established.     

Periodic variations of ionization rate in the low and middle atmosphere

The cosmic ray ionization source functions which were obtained using a simplified extensive air shower model are used to calculate the eleven year cycle, seasonal and diurnal variations of ionization rate in the low and middle atmosphere. The ionization source function, as a function of the penetrating depth and the energy of cosmic ray particles, is the ionization rate per unit depth for a unit flux of incoming cosmic ray particles with certain energy.The calculation of the eleven year cycle variation of ionization rate in the low and middle atmosphere due to the modulation of galactic cosmic ray intensity by solar activity shows that the amplitude is larger at a higher magnetic latitude and is generally larger at higher altitudes. The relative amplitude of fluctuation of the ionization peak value (at altitudes near 15 km) is up to 45% in the magnetic polar region. The ionization rate, due to the seasonal variation of the atmospheric density, varies from several per cent below the ionization peak to several tens per cent above the peak. This seasonal variation of ionization rate reaches 35% at 70 km. The diurnal variation of atmospheric densities caused by atmospheric tidal oscillation can produce a diurnal variation of the ionization rate to an amplitude of several per cent at altitudes above 40 km. The diurnal oscillation is less than 1% below 35 km.     

Comptel measurements of the omnidirectional high-energy neutron flux in near-earth orbit

On four occasions, twice in 1991 (near solar maximum) and twice in 1994 (near solar minimum), one COMPTEL D1 detector module was used as an omnidirectional detector to measure the high-energy (>12.8 MeV) neutron flux near an altitude of 450 km. The Dl modules are cylindrical, with radius 13.8 cm and depth 8 cm, and are filled with liquid scintillator (NE213A). The combined flux measurements can be fit reasonably well by a product of the Mt. Washington neutron monitor rate, a linear function in the spacecraft geocenter zenith angle, and an exponential function of the vertical geomagnetic cutoff rigidity in which the coefficient of the rigidity is a linear function of the neutron monitor rate. When pointed at the nadir, the flux is consistent with that expected from the atmospheric neutron albedo alone. When pointed at the zenith the flux is reduced by a factor of about 0.54. Thus the production of secondary neutrons in the massive (16000 kg) Compton Gamma-Ray Observatory spacecraft is negligible. Rather, the mass of the spacecraft provides shielding from the earth albedo.     

单推三分析化验误差来源研究

单推三分析化验误差来源是多方面的,确定单推三分析过程误差来源,能为操作人员提供减少或消除误差的依据。影响单推三分析结果的主要因素有几个:标准溶液浓度的变化,滴定过程各终点的读数,环境温度的变化。在分析化验过程中,第一终点读数对硝酸肼、氨的分析结果不产生影响,但对肼有影响;第二终点读数对肼、氨分析结果有影响,但对硝酸肼无影响;第三终点读数对上述三种物质的分析结果都有影响,尤其是硝酸肼,其分析化验结果很容易超出要求范围。     

便携式γ射线照射装置散射辐射特性研究

便携式γ射线照射装置对于提高固定式X、γ辐射剂量仪检定率、解决现场校准难题具有重要意义,利用蒙特卡罗模拟与实验测量协同开展便携式γ射线照射装置散射辐射特性研究。结果表明：蒙特卡罗方法可以模拟得到装置自身的散射辐射,实验测量只能获得照射装置以外辐射场中的散射辐射。利用MCNP程序F4卡和CF卡得到距放射源1 m处照射装置自身的散射贡献分别为13.07 %和4.55 %;反平方律实验和移出实验得到辐射场散射辐射贡献分别为0.2 %和3.94 %,满足ISO 4037-1:2019和GB/T 12162.1-2000的要求。该装置可用于固定式X、γ辐射剂量仪的现场校准。     

空间积分声光相关器——脉冲信号检测

论述了空间积分声光相关器对脉冲调制连续波信号的瞬时响应，分析了从实时光电检测器中检测出的波形，该波形是脉冲宽度，加权函数参量和与脉冲位置相关的空间衍射光分布的函数。进一步提出了脉冲序列相关时的光分布关系并通过实验加以论证。     

An experiment to study solar flare effects on radio-communication signals

The occurrence of radio signal fading events caused by ionospheric absorption plays an important role in the performance of radio-communication systems. It is necessary to know the magnitude and time-scale of such events in order to specify technical parameters of the communication system to be used. Generally, fading events are associated with solar flares, which are characterized by sudden increase in the solar X-ray flux that causes an increase in the ionization in the lower ionosphere. The abrupt increase of ionization causes the absorption of radio waves propagating in the Earth–ionosphere wave-guide and is reported as radio signal fading events. A simple experiment to monitor the behavior of lower ionosphere has been carried out at the Southern Space Observatory-SSO/INPE (29.43°S, 53.8°W), located in southern Brazil. The experiment is basically a computer controlled radio receiver that records the received signal strength of Amplitude Modulated (AM) radio signals in the HF (High Frequencies) range. We analyzed data of the 6 MHz beacon signal that has been transmitted by a broadcasting radio station located about 400 km from the observation site. In this work we present initial results of daily variation of the received signal strength and fading events associated with solar flares observed in the 6 MHz signal monitored by the experiment during 2001. X-ray solar flux data from the GOES-8 satellite were used to identify X-ray solar bursts associated with solar flares. Based on the one-year data collected by the experiment, a statistical summary of fading occurrences and their correlation with solar flares, as well as the distributions of time-scales and magnitudes of such events are presented.