应用iGMAS超快速星历的实时精密单点定位研究

中国主导建设的国际GNSS监测评估系统（iGMAS）相比国际上比较成熟的IGS系统在产品精度等方面存在差别，目前实时精密单点定位应用多采用IGS实时、近实时产品。为改变这一现状，针对iGMAS产品特性以及实时精密单点定位对超快速精密星历的需求，对iGMAS超快速星历的精度和稳定性方面进行评估，设计了iGMAS产品实时/事后下载应用程序，开展了基于iGMAS超快速星历的实时精密单点定位研究，并结合NovAtel OEM617双频接收机进行了GPS实时精密单点定位试验。实验结果表明，在连续观测23min后定位误差即可收敛到分米级，较接收机原始定位精度高一个量级，且稳定性好，最终在E/N/U方向定位误差均方根分别为7.2cm、6.4cm、15.2cm，与应用IGS超快速星历实时PPP试验取得相近的结果。研究实现了iGMAS数据获取、评估和实时PPP应用的一整套方案，验证了iGMAS超快速产品的性能，对推进iGMAS产品的应用提供了借鉴。     

嵌入式软件仿真测试环境软件体系结构研究

利用嵌入式软件仿真测试环境(ESSTE,Embedded Software Simulation Testing Environment)对实时嵌入式软件进行系统测试是国内外公认的、行之有效的方法.基于UML和"4+1"视图模型,系统地对ESSTE的软件体系结构进行了描述.各个视图之间保持了良好的一致性,特别地,在设计视图中将ESSTE软件分为两大组件-实时组件和非实时组件,并按照"管道-过滤器"的软件体系结构模式组织,分别给出了它们的关键类.非实时组件的关键类是配置工具类,实时组件的关键类是模型类、实时变量类和调度器类.据此设计和实现的ESSTE-Basic体现了较好的质量特性,如可更改性、可移植性等,其成功地对多个软件进行了系统测试,高效地发现了大量潜藏的软件错误,验证了ESSTE软件体系结构的正确性和有效性.     

复杂威胁环境下无人机实时航线规划逻辑架构

面向高对抗、强拒止的战场环境，实时航线规划是确保无人机（UAV）完成作战任务并提高自身生存概率的重要保障。为使无人机在面临不同程度的复杂威胁环境时能够选择合适的实时航线规划模式，提出了一种基于模糊推理机制的无人机实时航线规划逻辑架构。首先，对实时航线规划模式进行分类，从自主性的角度，重新划分人机权限分配等级，建立了实时航线规划模式与人机权限之间的联系；其次，针对典型观察—判断—决策—行动（OODA）循环存在“信任危机”的风险，构建了一种基于可变自主的实时航线规划体系架构，并对其逻辑进行了说明；最后，利用模糊推理机制实现了无人机系统动态人机权限分配，通过评判人机权限分配等级，进而确定实时航线规划模式。仿真结果表明:验证了实时航线规划逻辑架构的合理性和可变自主方法的有效性；经过综合分析，实时航线规划模式决策结果也比较符合实际作战需求；与模糊综合评价法相比，所提方法降低了人的主观性、实用性更强，得出的结果更加令人信服。      

BP网络实时图像自动选取算法研究

实时图像的自动选取是景像匹配自动化的关键技术.提出了一种基于神经网络的实时图像自动选取算法.仿真研究表明,引入Sobel算子的3层BP网络实时图像自动选取算法结构简单、训练时间短和分类准确性高,其并行处理能力能满足景像匹配技术的实时性要求.经最小二乘和Bayes精匹配算法检验,实时图经此网络选取、粗匹配和精匹配,可达到高于0.5像素的定位精度.     

实时嵌入式软件测试执行引擎的设计与实现

自动化的实时嵌入式软件测试中,测试描述执行系统的设计与实现是需要解决的关键问题之一.基于面向对象的思想,设计和实现了实时嵌入式软件测试描述语言的执行引擎.介绍了测试描述驱动的实时嵌入式软件自动化测试过程,并在此基础上提出了测试描述执行引擎的总体设计方案,阐述了编译过程和执行过程的实现方法,给出了符号表管理中哈希函数及其冲突的解决方法和基于SBRMS(Segment-Based Rate Monotonic Scheduling)调度策略的测试描述执行过程.对引擎的执行效率进行了评估和分析,结果表明,通过合理控制测试描述的规模和并发执行个数,测试描述执行引擎能够满足实时嵌入式软件自动化测试对实时、并发特性的要求,并具有良好的可移植性.     

紧缩场测试扫描架平面度控制系统研制

扫描架是紧缩场现场校准系统的关键测试设备。扫描架扫描平面度是影响校准准确度的关键指标。本文针对自研的扫描区域为φ6m的大型极化扫描架，设计了一套扫描架平面度实时补偿系统。该实时补偿系统可以实时检测扫描架扫描平面相对于基准平面的位置偏差，并通过伺服补偿机构完成补偿。测试结果表明该实时补偿系统可以准确、快速完成平面度的补偿，与半实时补偿方式相比具有更高的效率及精度。目前，该系统已成功应用于紧缩场现场校准。     

附加先验轨道约束的LEO几何法实时精密定轨验证分析

低轨卫星的实时精密定轨能够极大拓展其完成复杂科学任务的能力,例如实时环境监测、机动控制和卫星自主导航等.本文根据几何法实时精密定轨模型,提出了附加LEO先验轨道约束从而改善实时定轨的精度、收敛速度和稳定性的构想.分别采用广播星历、超快速星历预报部分和实时精密星历,设计了6种实时定轨方案,并利用Swarm-A,B,C星7天的观测数据进行方案验证与分析.结果表明,使用广播星历、IGU和IGC星历的方案精度递增,附加先验轨道约束能够进一步提升精度.使用IGC星历并附加标准差为1m的先验轨道约束后,在径向、切向和法向的定轨精度分别达到6.12cm,5.55cm和4.98cm.此外,附加先验轨道约束能够显著提升收敛速度,使用IGC星历平均收敛时间约为31min,附加标准差为1m的先验轨道约束后收敛仅需约4min.      

一个DIS实时通讯网络的设计与实现

以一个ＤＩＳ（分布交互仿真）实时网络的设计和开发过程为背景,研究了ＤＩＳ实时网络开发中的几个问题。在进行实时ＤＩＳ网络规划时,采用了多点传送的通讯服务方式,保证每个仿真应用只发送变化的信息,只处理与自身相关的信息。指出了进行数据的实时传输格式定义时应注意的几个问题,这些数据定义必须支持多种不同的操作系统和平台。最后给出了开发ＤＩＳ实时通讯软件的方法,包括通讯协议和应用编程接口的选择。     

GNSS实时动态授时精度分析

基于GNSS载波相位观测值的实时动态授时，可有效规避PPP授时对实时精密轨道和钟差产品的依赖问题，对短距离动、静态高精度时间用户具有重要意义。为了更好地验证GNSS实时动态授时性能，基于中国科学院国家授时中心时间频率资源和三个GNSS跟踪站长达2个月的观测数据，以GPS系统为例开展了授时试验。与事后PPP时间传递相比，实时动态授时结果差异STD优于0.15ns；与光纤双向时间传递结果相比，实时动态授时结果差异STD优于0.5ns。试验表明，GNSS实时动态授时精度能够达到亚纳秒量级，可为下一步推广应用提供重要参考。     

多级容错实时遥测定姿系统

介绍了风云二号卫星指令与数据获取站（ＣＤＡＳ）实时遥测定姿系统,该系统是一个采用多级容错、多处理器并发运行体系结构,统一实现包括精太阳脉冲解调在内的模拟遥测信号实时处理、卫星姿态实时确定、编码遥测信号解调和数据实时处理、卫星星－地回路仿真测试及系统大容量数据、图形、字符实时处理、通信、记录等多功能、长寿命、高可靠实时遥测定姿系统。     

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.     

陀螺仪短周期性能测试方法研究

讨论了陀螺仪短周期重复性能的标定测试方法,即极轴翻滚试验方法。该方法以地球极轴为基准,通过对一周过程的电流值进行离散傅立叶分析,经过相应的运算处理求出误差模型参数的估计值。试验结果表明,该方法辨识参数多,全面反映了陀螺仪性能,可以科学地考察陀螺仪的短周期重复性。     

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.     

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。      

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.     

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.      

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.     

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.      

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.