银河宇宙线在电离层D层中电离的全球分布

本文从带电粒子对D层大气电离出发, 给出了宇宙线相对论粒子、非相对论粒子及低能粒子在地球大气中的电离公式, 从而给出了宇宙线在电离层D层中电子产生率q(h)和电子密度N(h)的全球分布.结果表明, 宇宙线产生的q(h)和N(h)具有明显的纬度效应, 在极区产生的q(h)和N(h)要比低纬高得多, 当截止刚度R_c=10—18GV时, q(h)的变化相差很小.太阳活动11年调制对q(h)的影响是明显的, 但远小于R_c对q(h)的影响.大气密度ρ(h)对q(h)的影响主要是随高度的变化.      

Magnetic field disturbances in the mid-altitude cusp

Magnetic field disturbances and hot particles in the cusp as seen mainly by both the IMAP-3 magnetometer and PROMICS -3 spectrometer aboard the INTERBALL-AURORAL PROBE (AU) (perigee 4 Re, inclination 65 deg) are discussed. Orbits from March, 1997 are analysed accordingly. The INTERBALL-AU transits cross the middle of the cusp from low to high latitude from pre-noon to post-noon hours 11–13 MLT. Although the crossings are not exactly meridional, they reach 80–81 ILAT and permitting detection of the cusp, its subregions and their equatorward and poleward boundaries. Magnetic field disturbances are analysed for field-aligned currents (FACs) during different IMF conditions. Regions with structured forms are emphasised, in particular where a more intense current is concentrated. The following cases are compared: (a) the most intense current in the boundary cusp, adjacent to the ring current (March 7, southward IMF); (b) FACs are concentrated completely inside the cusp (March 13, southward -downward IMF) and (c) FACs with pronounced intensities equatorward from the cusp proper (March 11, duskward IMF).     

螺旋结构日珥与Kippenhahn-Schlüter模型

利用具有螺旋结构的宁静日珥观测资料,基于:(1)日珥内部的磁场位形具有无力性质;(2)日珥整体电流性质可用Kippenhahn-Schlüter模型描述;从理论上探讨了这些日珥的电流特性。并将所得结果与Kuperus-Raadu日珥模型进行了比较,结果表明:(i)日珥内部的磁场和电流确实具有无力性质;(ii)不考虑虚镜电流的Kippenhahn-Schlüter模型可能是描述宁静日珥电流特性的较好模型;(iii)可能存在两类导致日珥爆发的物理原因。      

电离层D区域电子浓度和电子有效损耗率随时间的变化

本文根据D电离层的电离复合理论,讨论了利用单站、单一频率的LF天波资料连续监测和研究D区域固定高度上电子浓度N(h₀,t)和电子有效损耗率ψ(h₀,t)随时间变化的方法。应用这一方法对武昌站的部分实验资料作了分析,得到了N(h₀,t)的日变化、月变化曲线;并发现ψ(h₀,t)也有明显的日照效应,上、下午呈现显著的不对称性;两者的逐日变化都较小。      

彗尾剪切磁流体的修正B—KdV方程及其非线性特征

本文运用二维约化摄动方程推导出彗尾剪彻磁流体的修正B-KdV方程,并定性讨论了其非线性性态。主要结论是:(1)推导出彗尾剪切磁流体修正的B-KdV方程,(2)给出彗尾宏观非线性波动与剪切背景的制约关系,(3)定性地解释了彗尾等离子体的一些复杂结构,(4)给出太阳风与彗尾等离子体相互作用的一种输运机制。     

状态监控与故障诊断聚类分析法

概要阐释聚类分析方法及其技术要点，对用聚类分析进行状态监控和故障诊断作了探索性研究，提出用８种系统聚类法进行状态监控和故障诊断。     

CORONAS-F observations of active phenomena on the sun

Complex observations in the framework of the CORONAS-F Mission aimed at the study of active phenomena inthe solar corona are described. The main features are given for the following experiments: (1) XUV-imaging spectroscopy with high temporal and spatial resolution, (2) X-ray spectroscopy, (3) X-ray and gamma-ray photometer/spectrometer, and (4) solar cosmic rays. Some new observational data on the structure and dynamics of flares and transient events are discussed along with their analysis.     

木星外磁层结构的定态模式

本文建立了描述木星外磁层结构的磁流体力学方程组,在这一方程组中考虑了磁层转速和等离子体片倾角(等离子体片与旋转赤道平面的夹角)随径向距离的变化。在不同条件下对此方程组求解,得出了等离子体片中各变量(磁场、压力、温度、质量密度和电流密度)的空间分布表达式。结果表明:各变量随Z(离开赤道平面的距离)的变化可用两种函数形式表示,一种是双曲线函数,这种分布形式与观测结果相符合;另一种是三角函数形式。各变量随径向距离r的关系是:压力P_o(r)～r-3.4,电流密度i_o(r)～r-1.7.对于绝热过程,密度ρ_o(r)～r-2.04,温度T_o(r)～r-1.36;对于等温过程,密度ρ_o(r)～r-3.4,温度T_o=常数。最后讨论了木星磁异常对外磁层结构的可能影响。      

Accuracy assessment of TDRSS-based TOPEX/Poseidon orbit determination

Orbit determination results are obtained for the Ocean Topography Experiment (TOPEX)/Poseidon spacecraft by the Goddard Space Flight Center (GSFC) Flight Dynamics Division (FDD) using a batch-least-squares estimator available in the Goddard Trajector Determination System (GTDS) to process Tracking and Data Relay Satellite (TDRS) System (TDRSS) measurements. The GTDS orbit solutions are compared with the definitive Precision Orbit Determination (POD) orbit solutions. The root-mean-square (RMS) solution difference in the radial component is 28 centimeters.     

一种微波及毫米波滤波器的精确设计方法

介绍了一种微波及毫米波滤波器精确设计方法:由滤波器的原型参数,导出滤波器的广义阻抗变换系数;采用模匹配法或耦合积分方程技术等数值算法精确计算各个耦合结的S参数,进而转换成广义阻抗变换系数;通过插值,获得满足原型要求的滤波器各个耦合结的结构尺寸以及谐振腔长度,将结构参数代入模匹配程序、HFSS或CST软件进行分析,分析结果与预期值一致。设计了26GHz矩形波导带通滤波器,模匹配法和HFSS以及CST软件的仿真结果、测试数据与设计要求一致,说明该种设计方法是有效的。     

Solar modulation and nuclear fragmentation effects in galactic cosmic ray transport through shielding.

Crews of manned interplanetary missions may accumulate significant radiation exposures from the galactic cosmic ray (GCR) environment in space. Estimates of how these dose levels are affected by the assumed temporal and spatial variations in the composition of the GCR environment, and by the effects of the spacecraft and body self-shielding on the transported radiation fields are presented. In this work, the physical processes through which shielding alters the transported radiation fields are described. We then present estimates of the effects on model calculations of (1) nuclear fragmentation model uncertainties, (2) solar modulation, (3) variations between solar cycles, and (4) proposed changes to the quality factors which relate dose equivalent to absorbed dose.     

地球磁鞘中磁场起伏特性的分布

本文利用行星际起伏通过激波后的变化的MHD模型, 具体讨论了地球磁鞘中磁场起伏特性在黄道面内的分布.主要结果是:(1)行星际磁场起伏的强度和各向异性在磁鞘中被显著放大;(2)行星际磁场基本位于黄道面内时, 磁鞘中磁场起伏特性(强度、相对起伏和各向异性等)呈现明显的晨一昏不对称性, 早晨侧(准平行激波)显著地高于黄昏侧(准垂直激波);(3)行星际磁场方向对磁场起伏特性在磁鞘中的分布有强烈的控制作用, 早晨侧响应灵敏, 黄昏侧反响不大.相对地讲, 黄昏侧的磁活动较之早晨侧稳定;(4)行星际磁场转南的增强将导致磁鞘中磁场起伏的最大区域自黄道面低纬向北极高纬移动, 南-北不对称性磁活动随之加强, 最强大致出现在磁场与黄道面相交成大约45°时, 而晨-昏不对称性的强弱程度则发生相反变化;(5)行星际磁场的相对起伏增加, 晨-昏不对称性反随之减弱.磁鞘中磁场起伏分布的特性与卫星观测大体符合, 是磁顶、边界层某些晨-管不对称性出现的可能起因之一.      

磁流体斜激波的碰撞

讨论了磁流体斜激波之间的碰撞及其与接触间断的相互作用规律,主要结论如下:(1)两个快激波碰撞后交换位置,同时出现一接触间断和一慢稀疏波对。(2)两个慢激波碰撞后交换位置且强度减弱,同时出现一接触间断和一块激波对。(3)一前向快激波与一后向慢激波碰撞后交换位置,快激波强度增加,慢激波强度减弱,同时出现一后向快激波、一负接触间断和一前向慢稀疏波。(4)一前向快激波与一正(负)接触间断相互作用后交换位置,快激波减弱,同时出现一后向快稀疏波(快激波)、一后向慢激波和一前向慢激波(慢稀疏波).(5)一前向慢激波与一正(负)接触间断相互作用后交换位置,慢激波减弱,同时出现一后向慢稀疏波(慢激波)和一快稀疏波(快激波)对。      

The AGN/normal galaxy connection: Summary

The connection between normal and active galaxies is reviewed, by summarizing our progress on answering nine key questions. (1) Do all galaxies contain massive dark objects (MDOs)? (2) Are these MDOs actually supermassive black holes? (3) Why are the dark objects so dark? (4) Do all galaxies contain an Active Galactic Nucleus (AGN)? (5) Are the “dwarf AGN” really AGN? (6) Does AGN activity correlate with host galaxy properties? (7) How are AGN fuelled? (8) Is AGN activity related to starburst activity? (9) How do quasars relate to galaxy formation?     

微光探测EMCCD在高灵敏度星敏感器中的应用研究

阐述了微光探测的主流技术,重点突出了电子倍增电荷耦合器件（EMCCD）的结构、功能和优点,并进行了噪声和信噪比分析。同时以星敏感器运用为目的,完成了这一部件的初步设计分析和计算。     

U.S. operational space program for climate observations

Satellites provide two important characteristics to earth climate studies not available from other, conventional sources: (1) full global coverage, and (2) consistency within the data set. This latter arises from the fact that the satellite data are usually derived from one instrument (or at least from a small number) whereas other sources involve large numbers of separate instruments and hence exhibit a substantial standard deviation. Satellite data, of course, are more subject to bias and must therefore be carefully validated, usually via ground truth.The ISCCP and ISLSCP are examples of the increasing reliance on satellite data for climate studies. In addition to the multispectral images, quantitative products of importance are: (1) atmospheric temperature structure, (2) snow cover, (3) precipitation, (4) vegetation index, (5) maximum/minimum temperature, (6) insolation, and (7) earth radiation balance. The U.S. civil space program is presently committed to its current geostationary (GOES) and polar (NOAA) programs through this decade and to continue both programs into the next decade with spacecraft carrying improved and augmented instrumentation. GOES VISSR Atmospheric Sounder (VAS) data, presently in research status and available only for special observation periods, will become available operationally in 1987 from the current spacecraft series. GOES-Next will provide additional spectral channels, simultaneous imaging, atmospheric soundings, and possibly increased resolution starting in 1990. The NOAA follow-on spacecraft, in the same time frame, is expected to provide additional spectral channels, improved passive microwave radiometry, and possibly increased spatial resolution. The Landsat program is expected to be continued by a commercial operator following the useful life of Landsat-5. All three follow-on programs are presently at various stages of definition and procurement. Final definition may not be completed until late in 1984. However, their status as of the time of this presentation will be reviewed in detail.     

MMS星座对磁层顶磁通量绳内离子惯性尺度结构的观测

利用MMS观测数据,对磁层顶通量绳内离子惯性尺度（d_i）的结构进行分析研究.结果发现,许多不同尺度（约1d_i至数十d_i）的通量绳内都存在具有d_i尺度的电流 j _m,其方向在磁层顶局地坐标系的-M方向,即与磁层顶查普曼-费拉罗电流同向,由电子在+M方向的运动（ v _em）携带.这些电流结构具有以下特征:磁鞘与磁层成分混合,磁场为开放形态;离子去磁化,电子与磁场冻结;N方向（即垂直于磁层顶电流片方向）的电场 E _n显著增大,幅度达到约20mV·m-1,并伴有明显的尖峰状起伏,该增强和尖峰状起伏的电场对应于霍尔电场.分析表明,电流、电子与离子运动的偏离以及霍尔电场之间遵从广义欧姆定律,三者密切关联.进一步对磁层顶磁重联的探测数据进行分析发现,在很多重联区内也存在与通量绳内相似的结构,其尺度约为d_i量级,其中霍尔电场 E _N、电流 j _M和电子速度 v _eM均与通量绳内对应物理量的方向相同且幅度相近.基于上述观测事实,采用经典FTE通量绳模型,对通量绳内电流、电子运动和霍尔电场的起源进行了初步探讨,认为其来源于磁层顶无碰撞磁重联区内的相应结构,并且后者在离子尺度通量绳的形成过程中起到重要作用.      

A review of 9-year performance and operation of the MOPITT instrument

The MOPITT (Measurements of Pollution in the Troposphere) instrument has provided more than nine years of global carbon monoxide (CO) measurements on a continuous basis since its launch aboard the Terra Spacecraft on December 18th, 1999. This paper gives an overview of the core sub-system performance and major issues of the in-flight instrument over the mission period. Some of the instrument anomalies are also discussed. The major successes are: (1) the concept of using a combination of correlation systems such as Length Modulated Cells (LMCs) and Pressure Modulated Cells (PMCs) to retrieve CO profiles in the troposphere; (2) the redundant design in the instrumentation which was crucial for coping with unexpected in-flight anomalies and for continuing the mission in the case of component failure; (3) the thermal environment on orbit that is so stable that some calibration procedures are not necessary; and (4) the recent production of CO total column retrieved from the MOPITT 2.3 μm channel.     

Mean winds of the mesosphere and lower thermosphere (60–110 km): A global distribution from radar systems (MF,Meteor, VHF)

During the last decade a large number of radars (～12) have been developed, which have produced substantial quantities of tidally-corrected mean winds data. The distribution of the radars is not global, but many areas are well covered: the Americas with Poker Flat (65°N), Saskatoon (52°N), Durham (43°N), Atlanta (34°N), Puerto Rico (18°N); Europe with Kiruna (68°), Garchy (47°N) and Monpazier (44°N); and Oceania with Christchurch (44°S), Adelaide (35°S), Townsville (20°S), and Kyoto (35°N). Zonal and meridional wind height-time cross-sections from $\text{60}\text{80}$ km (MF/Meteor Radar) to ～110 km have been prepared for the last 5–6 years. They are compared with cross-sections from CIRA-72 for zonal winds, and Groves (1969) for meridional winds.It is shown that while CIRA-72 is still a useful model for many purposes, significant differences exist between it and the new radar data. The latter demonstrate important seasonal, latitudinal, longitudinal and hemispheric variations. The new meridional cross-sections are of great value. The common features with Groves (1969) are the equatorward cells in summer near 85 km; however their strength (～10 ms^?1) and size are less. Systematic and somewhat different variations emerge at higher (?52°N) and middle (35–44°) latitudes.     

Mean winds of the upper middle atmosphere (∼70–110 km) from the global radar network: Comparisons with CIRA 72, and new rocket and satellite data

A substantial quantity of wind data have been assembled from radar systems since CIRA-72 was formed: most of these radars include height ranging, and operate on a regular and even continuous basis. Systems include meteor and MF (medium frequency) Radars: an MST (mesosphere-stratosphere-troposphere) Radar (meteor mode); and an LF (low frequency) drift system. Latitudes represented are near 20° N/S, 35° N/S, 45° N/S, 50°N, 65° N/S. In all cases tidal oscillations were calculated so that corrected mean winds (zonal, meridional) are available - the meridional was not included in CIRA-72. Means for groups of years near 1980 are available, as well as individual recent years (1983, 1984) to allow assessment of secular trends: revised and improved analysis has been completed for several stations.Height-time cross-sections have been formed for each observatory: heights are typically ∼75–110 km, with time resolution of 7–30 days. Such detailed cross-sections were almost unknown before 1972. Comparisons with CIRA-72 are shown, and these emphasize the differences between hemispheres (NH, SH) in the radar winds. Other new winds from rockets and satellite radiances are contrasted with the radar set. There are important differences with the satellite-derived geostrophic winds (1973–78): possible explanations involve secular trends, longitudinal variations, and ageostrophy.