自主火星离子与中性粒子分析仪数据压缩算法设计

火星离子与中性粒子分析仪共设计10种在轨探测模式，不同探测模式下数据率不同，多种探测模式下数据量远超出最大下行数据率的限制。为降低数据率，利用仪器内部FPGA有限的资源对压缩处理方法进行了详细设计。通过分析仪器数据特点，火星离子与中性粒子分析仪压缩算法采用合并处理、对数压缩和无损压缩三种压缩算法组合。对于每种探测模式，FPGA程序可根据压缩标志选择相应压缩算法，实现三种压缩算法串行使用，或选择其中一种或两种算法。并且压缩标志可通过注入指令改写，实现在轨时根据需求灵活配置。合并处理压缩比为2或4，对数压缩的压缩比为2，无损压缩效率与样本数据间的相关性有关。在此基础上，利用等离子体定标测试系统完成了地面测试。测试结果表明，各探测模式下科学数据经过压缩后数据率满足任务指标要求。     

Solar X-ray and EUV corona and their relation to the magnetic activity

We have studied the solar magnetic cycle in corona using X-ray data from YOHKOH and Extreme Ultraviolet data from SOHO/EIT. Soft X-ray data last the period from after the maximum cycle 22 to the maximum cycle 23 (1991–2001). The SOHO/EIT Extreme Ultraviolet data are used for the period from 1996 to 2003. These data provide us a unique opportunity to look at the solar corona on the solar disc and to compare with the magnetic activity, directly.Our studies reveal a close relationship between the coronal emissions and the photospheric magnetic field in the axisymmetrical case. The evolution of coronal structures in X-ray and EUV can be considered as a proxy of the coronal magnetic field and demonstrates a development of the solar magnetic cycle in corona. It is shown that the most important feature of the coronal cycle is the forming of giant loops structure visible in X-ray and, partially, in EUV (284A) on the solar disk.     

专用装备计量保障模式研究CSCD

结合目前装备计量保障现状,研究装备计量保障模式,对装备进行计量保障,重点掌握装备计量数据的准确性和任务条件下技术指标的可信性。从装备研制、生产、使用和维修阶段阐明进行计量保障必要性;从时效性出发,提出强制检定与系统测试相结合的计量保障方法;从可靠性出发,提出实验室计量检定与现场计量检定相结合计量保障方案;研究实现计量检定数据与系统测试数据共享,数据纵横向积累和分析研究的重要性。     

星载高速串行数据处理系统设计与实现

遥感卫星图像数据量的高速增长,以及遥感卫星搭载的相机不同工作模式下产生的数据差异化处理的需求,为星间数据处理带来了巨大挑战。针对星载Gbit·s^–1级高速数据收发及文件缓存等星间数据处理面临的问题,以百兆每秒级星载高速接收缓存系统为切入点,以遥感卫星数据处理的发展为依据,在分析SerDes传输原理的基础上,采用模型仿真和工程验证的方法,制定了高速串行数据链路层传输协议SSLLP(Satellite Serial Link Layer Protocol)和类文件化高速缓存的策略。在硬件设计和软件开发的基础上,最终完成了具备处理入口速率3.2 Gbit·s^–1并能以类文件化的方式缓存64个数据文件的星载数据处理单元的工程实现。测试结果表明,基于SSLLP的高速串行数据接收正确,缓存策略有效,系统高效可靠。该设计已在某型号任务中取得在轨验证,为星载高速串行数据处理系统提供了参考。     

Actual performance and capabilities of the Argos system

Since 1978, a new operational platform location system has come into being, namely the Argos system, which has the great advantage of bringing all results together at a single point. At the same time, this system provides for measurement data collection from platforms equipped with a simple electronics package, wherever they may be in the world.The data relayed by this system concern all environment-related disciplines, irrespective of whether we are referring to land masses, oceans, polar regions or the atmosphere.The central point where all location calculations are performed and all collected data handled is the Toulouse Space Center. Results are available at the Center just a few hours after their acquisition. Users can consult the results files via switched communications networks or have the data sent to them in one form or another.     

二维非结构网格的生成及其Euler方程解

 采用推进阵面法生成三角形非结构网格,用多重网格技术求解泊桑方程以取得结构背景网格.提出了一种高效的边界剖分法,并用它来生成初始阵面.另外,还提出了一种新颖的数据结构——数组链接表,用它来存贮网格数据.用有限体积法在非结构网格中求解了二维可压缩Euler方程,给出了单段翼型和多段翼型的算例,并与实验结果进行了比较和分析.     

数据链测试仿真评估中的信道与链路干扰仿真技术

信道和链路干扰仿真是数据链测试仿真评估系统的关键技术之一。在局域网下模拟数据链系统真实运行的无线环境的非理想特性,需要对典型应用环境的信道条件、干扰特征进行分析和建模,仿真验证数据链系统在不同环境条件下的性能。本文首先分析了几类常见的信道和链路干扰仿真工具相关模块的原理和机制,研究并提出了传输时延、信道与链路干扰、链路级仿真方法及方案,并对几个关键问题进行了分析并提出解决方案。该研究在数据链测试仿真评估系统中的验证效果良好,能够为数据链系统可靠性、稳定性提供无线信道和链路干扰模拟工具,从而为数据链系统的设计提供参考和依据。     

基于CAN总线的等效器的设计与实现CSCD

为了方便配合测量系统中某类部件的检测与监控,设计了基于CAN总线接口电路的等效器,增加了总线的监视功能和数据通信功能,从而实现了相关接口和功能电路的故障诊断功能。阐述了等效设备的CAN总线、数据采集测量以及数字IO功能。在实现全部功能的前提下,尽可能做到器件少、体积小,性能稳定可靠,并有效地实现测量系统综合检查的目的。     

Further information on structure of the atmosphere of Venus derived from the VEGA Venus balloon and Lander mission

Continued analysis of the pressure and temperature data returned by the two Vega mission balloons has revealed an apparently significant difference in mean atmospheric static stability between the two data sets. Furthermore, the stability is time dependent within each data set, as reported earlier. The 6.5K temperature contrast between the two balloons remains, and appears to have a counterpart in the contrast between two of the Pioneer Venus probes at these levels, which has been attributed to planetary scale waves. Comparisons of the Vega 2 Lander data with those of the Pioneer Venus Large Probe shows relatively close agreement in the state properties and in the atmospheric static stability profiles as well.     

星图仪数据的处理及其进一步应用

本文简述了星图仪数据处理的过程,并对如何进一步应用这些数据进行了探讨.我们知道,当星图仪对有一定亮度的恒星进行巡天扫描时,可获得一系列的时间信息量.当建立“卫星坐标系”,即以卫星自旋轴为坐标系的极,以垂直于自旋轴的平面为坐标系的基本平面时,则可以通过这些时间信息量,求得所扫到的恒星在“卫星坐标系”中的经纬度[1-3].      

Mesopheric structure and the d-region winter anomaly

Model mechanisms to explain the D-region winter anomaly have so far not really been successful, considering the many different aspects of this atmospheric/ionospheric phenomenon. A new model is therefore proposed relating the winter anomaly essentially to atmospheric temperature and wind variations. The new mechanism is checked by a set of data obtained during the Western European Winter Anomaly Campaign 1975/76, and additionally by a second set of data taken in earlier years.     

Study of the ionosphere during a magnetospheric storm using data on the ground and in space

For the magnetospheric storm of May 14–16, 1997 geophysical data of satellites DMSP and IMP-8 are compared with data of radio propagation on the high-latitude HF radio path of Heiss Island – St. Petersburg and data from European ionosondes. Peculiarities of variations of the operational frequencies range MOF–LOF (maximum and lowest observed frequencies) on the path were considered. The range has been determined by the method of oblique ionospheric sounding (OIS). The latter is more informative for observations during a magnetic storm compared to the vertical sounding method. Nevertheless, an analysis of variations of the critical frequency of the ionospheric F2 layer from the chain of European ionosondes was carried out. For interpretation of results, data of magnetospheric parameters, AE-indexes and riometer data were used. The variations of both frequency range on the path and critical frequencies of the F2 layer through the ionosondes chain during the disturbed period had certain regularities of behaviour. These regularities are being explained from the physical point of view. The analysis of the satellite DMSP data has showed that a magnetospheric disturbance causes displacement equatorward of precipitation and some growth of its width and energy.     

基于QoS真实性与工作流模型的Web服务选择

基于服务质量的Web服务选择方法往往假定服务提供者与使用者提供的质量数据均为真实可靠,而这一假设在实际中很难保证.为此,提出一种同时基于服务质量数据真实性与工作流模型的服务选择方法.对服务提供者发布的质量数据,根据服务运行数据的统计结果重新计算其客观质量值;对来自服务使用者的主观评价,通过工作流组织模型计算使用者间的信任度,并结合信任度计算当前用户的服务评价值.通过服务质量模型的建立,结合两种数据选出最优Web服务.实验证明该方法能够有效改善不可靠的质量数据对Web服务选择造成的影响,使服务选择结果更加准确.      

最新CCSDS图像压缩算法研究与实现

2005年CCSDS(空间数据系统咨询委员会)推出了一项新的图像数据压缩算法标准,制定算法标准的目的是为了解决有效载荷设备的数据压缩以及如何分段压缩能使地面更好地接收图像数据和解压缩.算法的应用能够减少静态图像的数据量,这样不仅可以降低传输带宽,减少数据存储,而且在给定码率情况下能缩短传输时间,这对空间数据压缩具有重要意义.针对CCSDS最新推出的图像压缩算法进行了研究并对其性能进行了阐述,分析了算法硬件实现的可行性,并将算法软件实现的结果与其他图像压缩算法的实现结果进行了测试比较,结果表明在低码率下压缩性能与JPEG 2000,SPIHT相当,甚至更好,完全符合星载图像压缩在低码率下传输的要求.      

星敏感器遮光罩消光比定量测试及数据处理方法

面向星敏感器在轨工作时的杂光抑制需求，开展星敏感器遮光罩消光比定量测试及数据处理方法研究。基于高灵敏度弱光探测组件、高精度电控转台以及太阳模拟器搭建杂光集成测试平台，在电控转台步进电机的驱动下实现不同光照角度时遮光罩消光比测量数据的实时获取。根据构建的数据处理模型计算获得遮光罩的消光比，并基于A类不确定度评定方法完成消光比测量的不确定度分析。从测量结果可以看到，在光照入射天顶角达到保护角30度时，消光比测量值达到10-6量级，在光照入射天顶角为54度时，消光比测量值达到10-7量级，且多次测量数据的变化规律基本一致。测量结果表明了测量方案的合理性和可行性，可为星敏感器系统方案设计、测试与评估提供重要的技术支持。     

飞行器自主保障系统海量数据存储设计与研究

随着飞行器数据规模扩大,数据存储成为核心技术。针对某飞行器地面自主保障信息系统海量数据存储需求,通过软件定义虚拟化存储,设计了一种采用完全对称架构和改进哈希算法的数据存储系统,系统无单点故障,具有很高的数据存储安全性,存储架构对称,容量可无限扩展,算法改进后,读写速度和负载均衡性能明显提高。     

基于多传感器天文信息的自主导航算法及可观测性分析

自主导航是未来航天器的发展趋势,利用由太阳敏感器、月球敏感器和红外地球敏感器组成的一体化多传感器天文观测平台,构建了多传感器的天文测量模型,结合航天器动力学模型,分析了自主导航系统的可观测性. 基于UKF滤波算法,建立多传感器自主导航算法,并采用原始测量信息和单点解析定位信息两种模式分别进行了仿真验证. 仿真结果表明,基于原始天文测量信息的自主导航模式,其导航精度要高于单点解析定位数据的自主导航精度,在无系统误差情况下,导航精度约为200m. 采用系统误差估计的自主导航方法后,常值系统误差对导航精度基本不产生影响.      

Rapid and Asymmetric Response of the Earth's Bow Shock:Multipoint Observations

We analyze observations of three bow shock crossings which occurred during 2007, using upstream data from STEREO A/B, ACE and WIND, combined with multi-point THEMIS and Cluster data, and TC-1 data located near noon. During the crossing of 7 May 2007, we find that following a rapid reduction in solar wind ram pressure and subsequent pressure pulse seen by ACE and WIND upstream, the bow shock responds asymmetrically from dawn to dusk. Cluster data on the dawn-side suggest the bow shock is significantly flared and responds rapidly to the pulse arrival, while TC-1 at noon, and THEMIS on the dusk-side, are well matched to the model bow shock, but show a delayed response. The crossings observed on 21 May and 2 June show contrasting response matching the model boundary for northward Interplanetary Magnetic Field (IMF). The IMF and solar wind plasma data suggest that the bow shock crossing at dawn-dusk side and subsolar point were mainly caused by large and smaller scale features of the solar wind ram pressure rise rather than the influence of IMF.      

Saturn radio emission and the solar wind: Voyager-2 studies

Voyager 2 data from the Plasma Science experiment, the Magnetometer experiment and the Planetary Radio Astronomy experiment were used to analyze the relationship between parameters of the solar wind/interplanetary medium and the nonthermal Saturn radiation. Solar wind and interplanetary magnetic field properties were combined to form quantities known to be important in controlling terrestrial magnetospheric processes.The Voyager 2 data set used in this investigation consists of 237 days of Saturn preencounter measurements. However, due to the immersion of Saturn and the Voyager 2 spacecraft into the extended Jupiter magnetic tail, substantial periods of the time series were lacking solar wind data. To cope with this problem a superposed epoch method (CHREE analysis) was used. The results indicate the superiority of the quantities containing the solar wind density in stimulating the radio emission of Saturn — a result found earlier using Voyager 1 data — and the minor importance of quantities incorporating the interplanetary magnetic field.