八毫米波段体效应管振荡源噪声特性测试方法的研究

本文介绍了测量微波振荡源近载频的频谱特性的各种方法。从频域方面着重叙述了微波振荡源的调频噪声、调幅噪声、谱线宽度的测量原理,测量方法,测量结果和各种注意事项。在时域方面介绍了微波振荡源的频率短期稳定度、长期稳定度、开机特性和温度特性等测量的原理和测量结果。得出的频域和时域的结果基本吻合。同时指出测调频噪声是评价微波振荡源的频谱特性最有效的手段。首次开展了八毫米波段国产体效应管振荡源的频谱特性和噪声参数的测试工作。     

一种用于液晶曝光中的激光检测系统

介绍了一种非接触式激光检测系统，可用于检测液晶曝光中液晶模板与基板之间的间隙，给出了该种系统的测量原理、硬件系统、信号处理方法、测量结果、分辨力和误差分析，并指出了这种测量系统的应用。     

红外无损检测加热不均时的图像处理方法

在红外热像无损检测中,为了减小加热不均的不良影响,提高缺陷对比度和检测深度,以碳纤维增强塑料试件的脉冲热像检测为例,研究了加热不均时的热像序列处理方法.分析和总结了加热不均产生的原因;提出了基于最小二乘法的去除拟合背景法、多项式拟合法及综合法等三种数据处理方法;通过实验对这三种处理方法进行了验证和比较;采用基于统计学的图像评估标准对处理效果作了定量评价.结果表明去除拟合背景法可有效地去除非均匀加热对缺陷识别的干扰,多项式拟合法兼有减小加热不均效应和增强缺陷对比度的作用,而综合法集成了前面二种方法的优点,可更显著地增强图像的缺陷对比度.     

八毫米细调谐振腔的设计

一、概述近年来毫米波技术已逐渐成熟,其应用也更为广泛了。因此毫米波元件的设计也将逐渐增多。随着频率的增高所设计的元件尺寸将越来越小,而零件的精度及光洁度要求则越来越高。例:1)园柱形腔体的尺寸——十厘米波段腔体的孔径根据不同要求可设计成几十毫米到一百几十毫米,但八毫米波段     

用于无线测量传输系统的双波段天线四功能馈源

双波段天线四功能馈源,属于改进的一种微波天线设备,可以同时传输C波段收、发信号和Ku波段收、发信号.通常的一副微波天线只接收一个波段的接收信号、并/或发射一个波段的发射信号.同时接收二个波段、发射二个波段的信号需要用二副天线,本设计可以用一副天线完成.本设计是将C波段馈源与Ku波段馈源通过串馈连接做在一个整体上,将它放在抛物面天线的焦点上,通过4个波导输出口与外部信号连接,实现双收、双发的功能.本设计不仅提高了经济效益而且节省了安装天线的占地面积,这对于天线安装在塔尖或房顶上是很重要的.     

航宇局的小型试验空间通信平台

图二,这是航宇局拟在八十年代中后期用航天飞机发射的小型空间通信平台。此试验平台长24.4米,可用一架航天飞机一次送入低地球轨道,然后再用其它助推器送入同步轨道。该平台可安装C波段、K_a波段、L波段和K_a波段的通信载荷。用6个这种平台在同步轨道上可完成目前124颗通信卫星所完成的通信业务量。详细报道见本刊1980年第七期第10页。     

双波段红外目标检测综述

红外成像系统具备优秀的夜间可视能力,并且具备良好的抗干扰能力、识别伪装的能力,在军事领域的应用日益广泛。可见光成像系统易受光照强度的影响,无法在封闭空间或夜间等弱光条件下工作,而物体的红外辐射能量仅与物体温度和物质特性有关,所以红外成像不需要考虑光照强度,可以在全天候时段工作。红外目标检测可以应用单波段和多波段的方式进行探测,单波段探测由于目标信息有限,往往目标会存在小、弱、暗等问题,导致检测能力不理想,而多波段检测通过利用不同波段信息的冗余性、互补性,大幅度提高目标检测和识别的概率,提高识别伪装的能力。但双波段目标检测中存在很多技术难点,对红外小目标检测技术进行了分类,分析了技术难点,按不同的方法进行了总结描述。再对双波段目标检测技术进行了详细的描述,并选取了常见算法进行了性能比较和原理分析,突出了双波段目标检测的优势。     

合成孔径聚焦在水浸超声缺陷定量中的应用

针对水浸超声检测常用缺陷定量方法存在成本高或缺陷定量误差较大的问题,提出一种将原始检测数据经频域合成孔径聚焦技术（FSAFT）处理后再运用半波高法进行缺陷定量评价（FSAFT-DQM）的新方法。建立了水浸超声点聚焦探头FSAFT成像方法,制备了横通孔和平底孔试样,开展了FSAFT-DQM缺陷定量评价试验研究。试验结果表明:FSAFT-DQM缺陷定量精度受检测深度影响不明显;当扫描步距不大于探头中心频率对应的半波长时,与半波高法相比,平底孔试样FSAFT-DQM缺陷定量误差由71.9%降低到10.0%以内;扫描步距在探头中心频率对应的半波长到波长之间时,图像频域插值算法将平底孔试样FSAFT-DQM缺陷定量误差由17.2%降低到5.6%。研究结果表明:FSAFT-DQM能有效提高缺陷定量精度。      

基于X波段雷达海浪监测装置的设计与研究

针对舰船对浪高实时测量的需要,提出了基于x波段雷达海浪监测装置的设计方案,具体介绍了基于X波段雷达海浪监测装置的设计原则、功能设计、硬件设计以及基于VC 的软件实现,并给出基于x波段雷达海浪监测装置系统操作平台功能界面的参考实例,从一定程度上为舰船海浪测量装置的实现与应用提供可行性参考。     

光栅式凸轮盘测量仪

主要用来检测各类机床预置功能部件——凸轮盘的功能曲线的形状误差和位置误差,可实现对凸轮盘的静态检测和动态检测。以被测件作为检测传动链的一个环节,可减少其传动误差,实现测量的连续性。由于采用长、圆光栅作为测量标准元件和定位元件,用计算机控制,用逻辑电路处理,从而可完成误差计数、自动显示、记录、绘图和打印等程序,具有较高的精度、检测效率和较多的测量功能。     

Research on the Relation Between the Seeker's Handover and the Geometrical Position of the Missile and the Target

 研究了雷达导引头的交班误差以及截获概率与交班时刻弹目几何位置的关系,提出了单个误差角的导引头天线指向角误差模型,它与两个误差角的导引头指向角误差模型相比可以更好地分析天线指向角误差,并得到使指向角误差最小的弹目几何位置;然后进一步得到使多普勒频率误差最小的弹目几何位置;给出了最终的截获概率的表达式,截获概率由目标处于导引头天线主波束的概率、目标回波多普勒频率落入接收机频带内的概率和目标的检测概率组成的;最后分析了一种典型的中末交班情况.     

Comparison of the magnetic field before the subsolar magnetopause with the magnetic field in the solar wind before the bow shock

Crossings of the magnetopause near the subsolar point are analyzed using data of THEMIS mission. Variations of the magnetic field near magnetopause measured by one of THEMIS satellites are studied and compared with simultaneous measurements in the solar wind by another THEMIS satellite. The time delay of the solar wind arrival at the subsolar point of the magnetopause is taken into account. 30 and 90 s averaging of the magnetic field in the magnetosheath is produced. The results of averaging are compared with the results of measurements in the solar wind before the bow shock and foreshock. It is shown, that _Bx$B_x$ component of the magnetic field near magnetopause is near to zero, which supports the possibility to consider the magnetopause as the tangential discontinuity. Comparatively good correlation of _By$B_y$ component in the solar wind and near the magnetopause is observed. The correlation of _Bz$B_z$ component near the magnetopause and IMF is practically absent, the sign of the _Bz$B_z$ near the subsolar point does not coincide with the sign of IMF _Bz$B_z$ in ∼$\sim$30% cases.     

Method for the prediction of the effective dose equivalent to the crew of the International Space Station

This paper describes a methodology for assessing the pre-mission exposure of space crew aboard the International Space Station (ISS) in terms of an effective dose equivalent. In this approach, the PHITS Monte Carlo code was used to assess the particle transport of galactic cosmic radiation (GCR) and trapped radiation for solar maximum and minimum conditions through an aluminum shield thickness. From these predicted spectra, and using fluence-to-dose conversion factors, a scaling ratio of the effective dose equivalent rate to the ICRU ambient dose equivalent rate at a 10 mm depth was determined. Only contributions from secondary neutrons, protons, and alpha particles were considered in this analysis.     

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.     

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.     

On the correlation of the solar wind observed at the L5 point and at the Earth

The L5 point is a promising location for forecasting co-rotating high-speed streams in the solar wind arriving at the Earth. We correlated the solar wind data obtained by the Nozomi spacecraft in interplanetary space and by the Advanced Composition Explorer (ACE) at the L1 point, and found that the correlation is significantly improved from that of the 27-day recurrence of ACE data. Based on the correlation between the two spacecraft observations, we estimated the correlation of the solar wind velocity between the L5 point and at the Earth, and found that the correlation coefficient was about 0.78 in late 1999, while that of the 27-day recurrence was 0.51. Eighty-eight percent of the velocity difference falls within 100 km/s between the L5 point and the Earth. This demonstrates the potential capability of solar wind monitoring at the L5 point to forecast the geomagnetic disturbances 4.5 days in advance.     

太阳风——磁层相互作用的磁流体力学数值模拟研究

磁层位于地球空间的最外层, 太阳风与磁层的相互作用是空间天气变化因果链中承上启下的关键环节, 是揭示地球空间天气基本规律的关键科学课题. 地球空间由于时变、多成分、多自由度的关联相互作用,使得传统的理论分析变得非常困难. 数值模拟作为近几十年发展起来的一个新的研究手段,对地球空间的理论和应用研究产生了深刻的影响. 国际上磁层的全球MHD数值模拟工作开始于20世纪70年代末, 最初的研究局限于二维空间. 由于磁层内在的三维特性, 20世纪80年代三维MHD数值模拟工作兴起. 本文简要说明了三维全球磁层MHD (磁流体力学)研究的特点及现状, 给出了三维全球磁层模型的基本框架, 综述了行星际激波与磁层相互作用、大尺度电流体系、重联电压和越极电位、磁层顶K-H不稳定性等方面的太阳风--磁层相互作用的MHD数值模拟的研究进展.      

辐射变色薄膜剂量计性能测试及加速器应用

本课题的目的是建立用于辐射加工高剂量水平吸收剂量测量的辐射变色薄膜剂量计。通过系统研究,批量制备了以尼龙为基材,副品红氰化物为染料的辐射变色薄膜剂量计。为了验证批制辐射变色薄膜剂量测量的可靠性,选择了国际上应用较广的FWT-60膜及丙氨酸薄膜剂量计与本实验室批制的辐射变色薄膜开展实验室内剂量比对,比对结果均在±4%内符合,归一化偏差En绝对值均小于1。通过在加速器上进一步应用实验表明批制辐射变色薄膜可用于电子束辐照参数测量。     

Influence of the Ionosphere on the Observation of the Mid-Latitude Pi2 Pulsations at the Global Scale

Results of our investigation showed that occurrence frequency of Pi2 over a 24 hour period undergoes seasonal variations in time coincidence with foF2. In the winter months, at sunrise and sunset (when foF2gradients are the largest) the observation probability of these oscillations is minimal. At periods of summer solstice when the F2-layer persists almost round the clock, no effect of Pi2 pulsation attenuation is observed at sunrise and sunset. The pulsation amplitudes behave in a similar manner. Results of this study suggest the conclusion that the propagation of signal from the Pi2 sourse into the mid-latitudes, and also the parameters of these pulsations are essentially affected by electron density in the ionospheric F2-layer.      

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.