紫外探测器光谱响应及噪声测量装置

介绍了紫外探测器相对光谱响应、绝对光谱响应、噪声测量装置,给出了测量结果,并进行了测量不确定度分忻。     

风云三号E星中能质子探测器标定

风云三号E星搭载的中能质子探测器实现了风云三号系列卫星首次对辐射带中能质子进行多方向的测量。中能质子探测器实现了对九个方向的测量能量范围为0.03～5 MeV的中能质子能谱的测量。为确定中能质子探测器的实际性能，在仪器交付前，利用中国科学院国家空间科学中心的中高能电子加速器，对中能质子探测器的能量分辨率，相对响应效率曲线、不同方向探头测量一致性以及抗电子污染能力进行了标定。文中介绍了仪器的标定场所、标定内容，并对标定的结果做了分析。其结果显示，仪器的能量分辨率为6.50%@310 keV，各测量一致性偏差优于1.51%，电子在仪器内产生污染计数的概率低于1%。该结果为中能质子探测器在轨运行时数据的分析处理提供了重要的参考依据。     

真空紫外探测器关键参数校准装置

当前真空紫外空间探测技术迅猛发展,真空紫外载荷应用越来越广,其中的核心器件真空紫外探测器的特性校准变得越来越重要,针对国内真空紫外探测器关键参数校准能力缺失问题,研制了一套真空紫外探测器关键参数校准装置,实现光谱响应率、线性度等参数的校准。论述了真空紫外探测器光谱响应率、线性度参数的校准方法,介绍了校准装置的硬件组成、校准方法和软件功能,并对其进行了测量不确定度评定。测试结果证明表明,该校准装置可以对真空紫外探测器进行主要参数的校准,校准结果准确、有效。     

基于双驱调制的高速光电探测器频响自校准表征

针对当前高速光电探测器频率响应测试的问题,提出了基于双驱调制的高速光电探测器频响自校准表征方法。该方法通过设置双驱调制频率为近似相等关系克服了电-光响应器件不平坦响应的额外校准,实现了光电探测器频率响应的自校准表征。同时,通过采用双驱调制频率的和频与差频拍频边带的相对功率来获得光电探测器的频率响应,摆脱了双驱马赫-曾德尔调制器偏置漂移的影响并扩展了两倍以上的测试带宽。相比于全光激励法,提高了测量精度与动态范围;与传统电光激励法相比,克服了强度调制器偏置漂移的影响和额外校准的难题;优于先前的双音调制法,简化了测试系统和降低了测量成本。光电探测器频率响应的实验测量结果与强度噪声法测量结果以及与该光电探测器出厂数据的一致性验证了该方法的正确性。     

脉冲激光测距误差标定及不确定度分析CSCD

以脉冲激光测距机的测距误差标定为背景,通过对测距误差解析表达式的推导,给出了系统各不确定度分量对测距误差的影响,计算了信号延迟时间、探测器和激光二极管响应时间、晶振频率、大气折射率等不确定度分量。通过对某已标定激光测距机实验验证表明:该装置在500m^20 000m测距范围内,测量重复性引入的相对标准不确定度最大值为0.67m,满足该类激光测距机测量不确定度5m(k=2)的校准测试需求。因此,利用该解析表达式可以实现对脉冲激光测距误差的有效评估,这对于脉冲激光测距测试系统、脉冲激光测距机的设计具有重要的指导意义。     

基于低温辐射计的探测器绝对光谱响应率测量

探测器的绝对光谱响应率是衡量光电探测器性能优劣的重要参数,直接反映其光电转化的能力。通过对低温辐射计,功率稳定系统光路调整的介绍,基于低温辐射计,对探测器可见光范围的7个波长的绝对光谱响应率进行了高精度测量,分析了测量结果。     

RRT对工业摄影测量基准尺精度影响研究

针对工业摄影测量基准尺在实际工程中实测值与标定值互差较大、比例缩放不准确等问题，以RRT为研究对象，推导出了基准长度误差模型。从RRT圆度、中心定位稳健性、基准尺长度标定一致性以及标准长度测量等方面进行了试验研究。通过研究发现，模切覆膜型RRT圆度和中心定位稳健性远高于其它类型的RRT。模切覆膜型RRT基准尺长度标定间的重复性为1μm,优于印刷型RRT基准尺长度标定的重复性。采用模切覆膜型RRT基准尺对标准长度的测量误差较印刷型RRT基准尺小约33%。选择模切覆膜型RRT作为基准尺的基准靶点对于提高工业摄影测量系统的测量精度具有重要参考意义。     

近红外绝对光谱响应度传递标准的研制CSCD

在光辐射计量中,陷阱探测技术是一种重要的探测技术,陷阱探测器是光辐射功率基准量值保持和传递的主要媒介。 InGaAs 陷阱探测器常被作为（900～1700）nm 波段光辐射计量的传递标准。本文基于陷阱探测技术,针对近红外波段量值传递的需求,研制了 InGaAs 陷阱探测器,并进行了性能测试。测试结果显示：在1064nm处绝对光谱响应率为0.7098A/ W,测量不确定度达到0.1%,在（0.1～3） mW 内,其非线性指标优于0.99993,1h 测试非稳定性为0.00495%,空间非均匀性达到0.05%,满足作为传递标准的技术要求。     

回归反射球基准尺校准技术研究

回归反射球基准尺广泛应用于数字近景摄影测量系统的标定。提出了一种回归反射球基准尺校准方法,建立了由三路激光干涉仪、高分辨率双远心成像瞄准模块、高精度直线气浮运动机构等组成的测量系统。对名义值为500mm、1000mm、1500mm、2000mm的4种规格回归反射球基准尺进行了长度测量实验,结果表明该方法可以满足回归反射球基准尺的校准要求。     

空间调制光谱成像仪相对辐射校正方法研究

空间调制干涉光谱成像仪不同于其他类型光谱成像仪,其得到的是包含地物空间信息和光谱信息的立方体干涉数据。该光谱成像仪由于原理特殊,在轨数据定标方法尚不成熟。文中介绍了一种基于统计思想来计算探测器CCD辐射模型的在轨相对辐射校正方法,并通过对"环境一号"A卫星上测得的实际在轨数据进行相应的处理,来验证该相对辐射校正处理效果。结果表明该方法可以达到修正CCD响应不均匀性、光场不均匀性和减小非线性相位偏移的双重作用,提高复原光谱的精度。     

Consequences of the application of the streamer fluid model to the study of the sprite inception mechanism

We present the results of a streamer-fluid model used to investigate the electrodynamical coupling between the troposphere and upper atmosphere due to the penetration of lightning electric fields into the mesosphere and the lower ionosphere, generating sprites. The model solves the continuity equation for electrons and ions coupled to Poisson equation. The dominant physical response of the atmosphere is the formation of a screening-ionization wave. The wave shields the atmosphere above it from the action of the lightning field and, together with the conductivity reduction below it due to attachment, the wave amplifies the total field below it, allowing for the penetration of intense electric fields in the mesosphere as it propagates downwards into regions of higher density that compress the wave. This is the key physical mechanism for sprite inception. We evaluated the effects of the thundercloud charge geometry, lightning current waveshape, atmospheric conductivity, via different electron density profiles, and the effect of ionization, attachment and electron mobility coefficients in the electrical breakdown process, related to halo production, and sprite streamer initiation. The results showed that electrons with higher mobility are more efficient in shielding the lightning electric field before breakdown, causing delay, and they contribute to the formation of the streamer seed after breakdown, anticipating the sprite streamer inception. Similarly, a higher effective ionization rate, produced by modifications in the attachment and ionization coefficients, anticipates sprite inception. The simulations with 6 different electron density profiles, and therefore conductivities, spanning 4 orders of magnitude, showed that the altitude of breakdown and sprite initiation, as well as their time delays from the lightning discharge are directly related to atmospheric conductivity: higher conductivities produce halo and sprite inception at lower altitudes with longer delays and may hinder sprite formation. We document that variations of 30 times in the lightning current leads to sprite initiation altitudes in the range 66.0–73.5 km, with delays between 1.550 and 34.500 ms, while variations of 4 orders of magnitude in the conductivity profile lead to initiation altitudes 61.0–70.6 km, with delays in the range 3.825–9.825 ms. Consequently, we suggest that lightning characteristics dominate over atmospheric parameters in determining sprites’ initiation altitude and delay. The simulation of a −CG, with a constant current of 30 kA, did not produce a sprite seed, confirming an asymmetry in the response of the atmosphere to positive and negative lightning. This is due to the free electron drift direction that is away from the screening ionization wave, preventing the formation of the streamer seed for the great majority of −CGs. The same does not apply to halos, which depend on the occurrence of breakdown and can be produced by discharges of both polarities.     

电离层电场对磁层活动响应时延的模式研究

本文用极盖边界上电离层驱动电位φ₀随时间变化的不同模式计算了场向电流J_∥2及电离层对流电场E的演化过程。计算表明,当φ₀(t)先升后降有极大值时,J_∥2(t)和E(t)也表现出类似的趋势。但它们的极值滞后于φ_0max出现的时刻,即在一段时间内,φ₀虽已开始下降,J_∥2及高纬E却继续增大。一般说,E先于J_∥2达到极值,但相差甚小。φ₀变化形式不同时,滞后时间亦不同。当φ₀陡升缓降时,E、J_∥2的极值相对于φ_0max的时延可超过一小时。这与持续时间较长的磁暴期间所观测到的电离层场强响应时延量级是一致的。时延大小还受电离层电导率的制约。低纬电离层场强的响应与高纬不同,其升降趋势与φ₀同步。      

Comprehensive investigation of the basic parameters of the upper atmosphere at the time of the flight of the geophysical rocket “vertical-6”

Ion temperature and total ion concentration measured on 25th October 1977 during the flight of the geophysical rocket “Vertical-6” are analyzed. The solar EUV fluxes determined in five wave-length bands with a photoelectron analyzer are also given. The observed anomalous variation of ion temperature between 700 and 900 km and the measured ion concentration can be explained, if the charge exchange reactions H⁺ ? O⁺ and diffusion are taken into account.     

落塔微重力水平激光干涉测量方法中的干扰因素分析

落塔是获得微重力环境的重要设施,落塔微重力水平的测量对微重力科学实验的研究至关重要. 激光干涉是测量落塔微重力水平的一种新方法,这种方法的基本原理是让一个参考落体在落舱中自由下落,落舱由于受到服外空气阻力的作用将与自由落体运动略有差异,1 11. 肫内的参考落体则更接近理想的自由落体运动,这就使得落舱与参考落体之间存在着加速度差,这种加速度差便反映了落服的微重力水平,其所导致的相对运动则可通过激光干涉的方法测量出来. 本文对落塔微重力水平的激光干涉测量方法中将会遇到的一些主要干扰因素进行了分析,计算结果表明,这些干扰网素所造成的总误差约为 1.2 x 10-7g,低于微重力水平的预测值 10-4~lO-6 g,因此该方法是一种比较可行的测量方法.      

热流效应对场向电流确定的影响

给出了任意速度分布函数条件下复频率的介电函数和色散关系的求解方法. 讨论了16矩近似条件下, 场向热流对电子速度分布函数, 介电函数实部与虚部, 以及离子与电子谐振频率和阻尼率的影响, 并与平衡态时麦克斯韦分布等离子体的计算结果进行了比较. 忽略场向热流效应, 正向电子漂移速度条件下, 上行等离子线探测, 会过高估计场向电流; 负向电子漂移速度条件下, 上行等离子线探测会过低估计场向电流. 对上下行等离子线同时探测情况, 忽略热流效应同样会过高估计场向电流.      

推力架测试系统误差的研究

针对卫星推进系统小推力测量的特点,主要是分析推力架系统所带来的推力误差,对引起推力误差的因素进行了分析研究,并提出了误差相应的解决方法和试验数据处理方法     

Possible physical properties of the flow in the vicinity of the heliopause

An interface between the fully ionized hydrogen plasma of the solar wind (SW) and the partially ionized hydrogen gas flow of the local interstellar medium (LISM) is formed as a region where there is a strong interaction between these two flows. The interface is bounded by the solar wind termination shock (TS) and the LISM bow shock (BS) and is separated on two regions by the heliopause (HP) separating the solar wind and charged component of the LISM (plasma component below). The BS is formed due to the deceleration of the supersonic LISM flow relative to the solar system. Regions of the interface between the TS and HP and between the HP and BS were in literature named as the inner and outer heliosheaths, respectively. An investigation of the structure and physical properties of the heliosheath is at present especially interested due to the fact that Voyager-1 and Voyager-2 have crossed the TS in December 2004 (Burlaga, L.F., Ness, N.F., Acuna, M.Y., et al. Crossing the termination shock into the the heliosheath. Magnetic fields. Science 309, 2027–2029, 2005; Fisk, L.A. Journey into the unknown beyond. Science 309, 2016–2017, 2005; Decker, R.B., Krimigis, S.M., Roelof, E.C., et al. Voyager 1 in the foreshock, termination shock and heliosheath. Science 309, 2020–2024, 2005; Stone, E.C., Cummings, A.C., McDonald, F.B., et al. Voyager 1 explores the termination shock region and the heliosheath beyond. Science 309, 2017–2020, 2005) and in September 2007 (Jokipii, J.R. A shock for Voyager 2. Nature 454, 38–39, 2008; Gurnett, D.A., Kurth, W.S. Intense plasma waves at and near the solar wind termination shock. Nature 454, 78–80, 2008. doi: 10.1038/nature07023; Wang, L., Lin, R.P., Larson, D.E., Luhmann, J.G. Domination of heliosheath pressure by shock-accelerated pickup ions from observations of neutral atoms. Nature 454, 81–83, 2008. doi: 10.1038/nature07068.14; Burlaga, L.F., Ness, N.F., Acuna, M.H., et al. Magnetic fields at the solar wind termination shock. Nature 454, 75–77, 2008. doi: 10.1038/nature07029; Richardson, J.D., Kasper, J.C., Wang, C., et al. Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock. Nature 454, 63–66, 2008. doi: 10.1038/nature07024; Stone, E.C., Cummings, A.C., McDonald, F.B., et al. An asymmetric solar wind termination shock. Nature 454, 71–74, 2008. doi: 10.1038/nature07022; Decker, R.B., Krimigis, S.M., Roelof, E.C., et al. Mediation of the solar wind termination shock by non-thermal ions. Nature 454, 67–70, 2008. doi: 10.1038/nature 07030), respectively, and entered to the inner heliosheath.     

火星地形对火星大气运动的影响及火星尘暴发生的可能机制

本文在准地转模式的假定下,讨论了火星地形对火星大气的影响,并根据文章所提供的信息对火星尘暴发生的物理机制作了粗略的解释。      

Testing the improvement of performance of the IRI model in the estimation of TEC over the mid-latitude American regions

This paper mainly discusses the improvement of performance of the International Reference Ionosphere (IRI) model in estimating the variation of the Vertical Total Electron Content (VTEC) over the mid latitude American regions during the relatively low (2008–2010) and relatively high (2012) solar activity years. This has been conducted employing the VTEC values obtained from the dual frequency ground based Global Positioning System (GPS) receivers located at Mineral Area Community College, MACC (37.85°N, 269.52°W) and Mississippi County Airport, MAIR (36.85°N, 270.64°W), and the latest versions of the IRI online model (IRI 2007, IRI 2012 and IRI 2016). The study mainly focuses to compare the trend of variability of the monthly and seasonal modeled VTEC values (IRI 2007 VTEC, IRI 2012 VTEC and IRI 2016 VTEC) with the corresponding measured VTEC values (GPS VTEC). The overall results show that the IRI VTEC values (almost in all versions of the model) are generally smaller than the GPS VTEC except after about 15:00 UT (09:00 LT) in the December solstice when the Sun shifts to the high solar activity. On the contrary, overestimations of the VTEC values by the model are observed in traversing from the low solar activity (2008) to high solar activity (2012) phase, especially after about 15:00 UT (09::00 LT) with the IRI 2016 version showing the highest. In general, the IRI 2007 and IRI 2012 versions show similar monthly and seasonal underestimations or overestimations showing that the two versions have almost similar performance. The IRI 2016 version is generally better in capturing both the diurnal and arithmetic mean GPS VTEC values with some exceptional months and seasons as compared to those of the IRI 2007 and IRI 2012 versions.     

Features of the occurrence of the additional stratification on the bottom-side F region over the equatorial location of Trivandrum

The general features of occurrence of an additional layer on the bottom side of F region, referred to as F0.5 layer in the pre noon period, over the magnetic equatorial location of Trivandrum (8.5° N; 77° E; dip lat of 0.5° N) in India during the period from 2004 to 2007 are presented using ionosonde observations. The F0.5 layer has a June (northern summer) solsticial maximum probability of occurrence with secondary maxima during December (northern winter) solstice. The seasonal as well as the day-to-day variability in the occurrence of F0.5 layer as mentioned in this paper seems to be a result of the variations in the amplitude and phases of the tides and gravity waves, and inventory of the metallic ions of meteoric origin. This study brings out an important manifestation of morning time F layer base region dynamics.