等效导纳模型分析航天器VHF/UHF频段屏蔽效能

针对VHF/UHF频段航天器舱体屏蔽处理难度大的问题,提出一种基于等效导纳模型的屏蔽效能分析方法。该方法将屏蔽舱体孔缝等效为波导结构,基于变分法原理建立水平电容和垂直电感模型,对参数失配和舱体厚度影响进行导纳匹配和孔缝宽度参数修正。采用传输线理论建立屏蔽效能分析数学模型。算例对比表明算法具有较高的分析精度,可有效分析孔缝不位于舱体中心位置和孔缝长度非波长整数倍时的屏蔽效能,并可准确预测舱体的谐振效应。将其应用到航天器舱体屏蔽效能分析中,对比结果表明算法可有效满足工程应用要求。     

基于VHF数据链的自动相关监视系统

介绍了基于甚高频(VHF)数据链的自动相关监视(ADS)系统的基本概念,构成原理和系统结构.为改善ADS系统的跟踪精度,将基于"当前"模型的卡尔曼滤波算法用于ADS系统数据处理.数字仿真和实际应用表明:该算法可以有效地消除由于突发干扰和飞机姿态变化造成的ADS报文丢失、乱码对ADS系统跟踪精度的影响,使ADS系统更为实用化.      

Simultaneous observations of spread F irregularities over Southeast Asia longitude using Sanya VHF radar,GPS and C/NOFS

Through concurrently measurements by Communication/Navigation Outage Forecasting System (C/NOFS), Sanya VHF radar and GPS ionospheric scintillation receiver on 12 March 2010, five plasma bubbles were found and three of them were observed by all those instruments. Two well-developed plumes with strong backscatter echoes were measured by Sanya radar and their corresponding depletions were observed by C/NOFS in Orbit 10317, 10318 and 10319. Broad plasma depletions resulting from merging process were found in orbit of 10318. The occurrence time and geophysical positions of scintillations correlate well with observations implemented by Sanya VHF radar and C/NOFS. Observations from three types of instrument indicate that the spread F irregularities have distinct scale. There were longitudinal differences between Sanya VHF radar and C/NOFS as irregularities measured, and the eastward drift of developed bubbles are responsible for these differences.     

极区夏季中间层半日潮汐的VHF雷达观测

采用德国SOUSYVHF雷达观测数据,研究了极区夏季中间层半日潮汐的结构和变化特征.纬向和经向风的动态Lomb-Scargle谱表明,半日潮是中间层高度上占支配地位的波动,其谱峰对应的频率一般与1/12c·h-1有偏离,说明它们经常处在被扰动状态.稳定的半日潮振幅随高度增加而迅速增长,在87.9km高度附近达到饱和;经向分量的相位一般比纬向分量的相位超前π/4-π/2,从而水平扰动速度矢量端点随时间变化的轨迹显示出顺时针方向旋转的特征.半日潮汐特征参量在纬向和经向风中随时间的变化在基本趋势一致的基础上显示出一定程度的各向异性.      

Morphological studies on ionospheric VHF scintillations over an Indian low latitude station during a solar cycle period (2001–2010)

The amplitude scintillations data recorded at 244 MHz from the geostationary satellite, FLEETSAT (73°E) at a low latitude station, Waltair (17.7°N, 83.3°E) during the ten year period of high to low solar activity from 2001 to 2010 is considered to study the occurrence characteristics of the VHF scintillations. A close association between the intense scintillations on VHF signals during pre-midnight hours, associated with range type of spread-F on ionograms and a relatively weak and slow fading scintillations during post-midnight hours associated with frequency type of spread-F is observed during the relatively high sunspot years from 2001 to 2004, whereas during the low sunspot years from 2005 to 2010 the scintillation activity as well as spread-F activity are found to be minimum. During both the high and low sunspot years, it is observed that the maximum scintillation activity occurs during equinoctial months followed by winter with the minimum occurrence during summer months. The annual mean percentage occurrence of scintillations is found to be clearly associated with the variations in the annual mean sunspot number. The nocturnal variations in the occurrence of scintillations show the onset of scintillation activity starts from 19:00 h LT with maximum of occurrence around 21:00 h LT. A clear semiannual variation in the occurrence of scintillations is observed during pre-midnight hours with two peaks in equinoctial months of March/April and September/October. The number of scintillation patches observed is found to be more during pre-midnight hours compared to those during post-midnight hours. The most probable scintillation patch duration lies around 30 min. Further, it is also found that the number of scintillation patches with durations of 60 min and more decreases with the increase in the patch duration. It is also observed in general that the scintillation activity is inhibited during geomagnetic disturbed days.     

甚高频空地数据链信道访问模型及性能分析

在建立甚高频空地数据链信道访问状态模型的基础上,利用连续时间的马尔可夫链模型和ＣＳＭＡ矩阵分析方法,分析了空地数据包试图发送率、信道传输检测时间对数据链性能的影响,对不同用户访问规律、不同的数据包发送用户数下的信道吞吐量和报文数据延时等性能指标进行数值模拟,结果表明,用户数目、重传率及信道检测时间对数据链性能有显著影响。     

基于信道估计自适应算法的AVLC重发机制仿真

航空甚高频链路控制(AVLC)是下一代民航地空数据链甚高频数据链模式2(VDL2)的链路服务规程.为了提高AVLC重发控制效率、减少误重发,提出了基于信道估计的监督帧发送时刻自适应算法.在OPNET平台上建立了物理层、数据链路层和子网层VDL2架构;利用动态进程建模方法,建立了AVLC模型.通过对无监督帧、监督帧发送时刻静态算法和自适应算法分别建模,开展对比仿真,验证了监督帧重发控制对于提高VDL2性能的有效性和自适应算法较静态算法的优越性.实验结果表明,在宽范围的系数合理区间内,所提出的算法可有效增加吞吐量,缩小包延时,同时可增强系统稳定性.      

甚高频空地数据链的通信链接控制模式分析

通信链接控制模式与甚高频 ( VHF)空地数据链的性能、系统容量和系统冗余度密切相关,采用嵌入式马尔可夫模型,详细分析了目前正在使用的两种典型的通信链接控制模式对空地数据链性能的影响,进行了计算机仿真,对分析结果进行了比较研究,并以此提出一种有效的新型通信链接控制模式。     

Low latitude ionospheric scintillation and zonal irregularity drifts observed with GPS-SCINDA system and closely spaced VHF receivers in Kenya

In this study we have used VHF and GPS-SCINDA receivers located at Nairobi (36.8°E, 1.3°S, dip −24.1°) in Kenya, to investigate the ionospheric scintillation and zonal drift irregularities of a few hundred meter-scale irregularities associated with equatorial plasma density bubbles for the period 2011. From simultaneous observations of amplitude scintillation at VHF and L-band frequencies, it is evident that the scintillation activity is higher during the post sunset hours of the equinoctial months than at the solstice. While it is noted that there is practically no signatures of the L-band scintillation in solstice months (June, July, December, January) and after midnight, VHF scintillation does occur in the solstice months and show post midnight activity through all the seasons. VHF scintillation is characterized by long duration of activity and slow fading that lasts till early morning hours (05:00 LT). Equinoctial asymmetry in scintillation occurs with higher occurrence in March–April than in September–October. The occurrence of post midnight VHF scintillation in this region is unusual and suggests some mechanisms for the formation of scintillation structure that might not be clearly understood. Zonal drift velocities of irregularities were measured using cross-correlation analysis with time series of the VHF scintillation structure from two closely spaced antennas. Statistical analyses of the distribution of zonal drift velocities after sunset hours indicate that the range of the velocities is 30–160 m/s. This is the first analysis of the zonal plasma drift velocity over this region. Based on these results we suggest that the east–west component of the plasma drift velocity may be related to the evolution of plasma bubble irregularities caused by the prereversal enhancement of the eastward electric fields. The equinoctial asymmetry of the drift velocities and scintillation could be attributed to the asymmetry of neutral winds in the thermosphere that drives the eastward electric fields.