星载GPS接收机RAIM算法性能及参数影响分析

为提高星载GPS接收机的故障鉴别与故障隔离能力,研究了星载接收机自主完好性监测(RAIM)算法的性能,以及参数选取对性能的影响;给出了RAIM算法的可用性及RAIM算法应用的可靠性衡量指标,并推导了内、外灵敏度的计算方法。设计了2种适合于高动态在轨应用环境的参数场景,并基于这2种场景,利用在轨数据分析了性能之间的相互制约关系及不同参数对性能的影响。仿真结果表明:若定位告警门限取300m,可以保证90%的RAIM算法可用性;对于20m的测量误差,能够保证80%的检测概率。将不同性能与先验参数的影响关系具体化,可为不同环境、背景下RAIM算法在工程应用中的参数选取及性能评估提供参考。     

基于贝叶斯因子和二阶概率方法的圣地亚热传导模型确认挑战问题

针对美国圣地亚国家实验室为促进模型确认方法的发展所提出的热传导挑战问题,根据现代模型确认思想总结了该挑战问题解答中应包含的核心内容。在确认度量环节采用贝叶斯因子考察了实验数据是否支持所给模型,在此基础上通过二阶概率方法得到了模型预测的分布,以此计算出模型预测结论的置信度。该过程中考虑了模型参数的随机不确定性和认知不确定性,最后通过灵敏度分析辨识了模型参数的不确定性对模型预测的影响。研究表明该挑战问题中的实验数据支持所给模型,模型预测受导热系数的不确定性影响最大,模型预测材料在调控条件下的失效概率不满足调控要求,该结论的置信度为99.97%。     

基于概率的航空发动机飞行换算率改进算法

针对斯贝MK202发动机应力标准对零部件工作寿命评定中未包含各种随机因素的影响,考虑零部件疲劳性能参数的分散性和发动机整机载荷谱的随机性,将实测数据统计分析、零部件应力有限元分析以及蒙特卡罗模拟分析有机结合,提出了基于概率的航空发动机飞行换算率改进算法,以解释航空发动机零部件实际工作寿命存在的差异.经范例验证表明:确定性寿命评定方法的飞行换算率计算结果与改进算法下的平均值相当;对于单次飞行换算率,改进算法的单次飞行换算率平均值比确定性方法的计算结果小2%;对于综合飞行换算率,改进算法的综合飞行换算率平均值比确定性方法的结果小1%;且在改进算法下单次飞行换算率和综合飞行换算率服从正态分布.     

基于全报废模型的航空发动机叶片报废率预测方法

基于航空发动机叶片的全报废数据,建立了发动机叶片报废率威布尔分布模型,并运用中位秩的方法对威布尔模型的参数进行了求解。为验证所建立模型的有效性,运用某航空公司CFM56-7B航空发动机报废率数据对模型进行了验证,取得了较好的效果。所建立的报废率模型能够为航空发动机的送修目标确定、维修工作范围制定等提供理论的支持。     

基于概率统计的DS/FH系统干扰检测算法

基于时频分布的干扰检测算法是DS/FH（Direct Sequence/Frequency Hopping,直接序列扩频/跳频扩频）系统干扰检测的传统手段,针对其运算量大、实时性差,以及无法检测某些特殊干扰信号等问题,提出一种基于概率统计的干扰检测算法.通过统计DS/FH系统频谱图中各频率的幅值出现位置,以DS/FH信号与干扰信号频谱分布规律的差别为判决依据,完成DS/FH系统中干扰信号的检测.分析和仿真结果表明：该检测算法能够有效识别DS/FH系统中的典型干扰信号,与传统基于时频分布的检测算法相比,能够实现某些特殊干扰信号的有效检测;同时,由于该算法不需要进行复杂的时频联合分析,其运算复杂度大大降低,能够实现DS/FH系统干扰信号的快速检测.     

基于相关系数的火箭测试变化缓变参数自动判读方法

变化缓变参数的自动判读是实现火箭测试数据自动判读的难点,已有的研究采用曲线拟合的思路进行判读,但拟合过程相当复杂,且不同的测试流程存在不同的拟合曲线,工作量极大.为提高判读效率,从变化缓变参数的物理意义出发,提出通过判别参数测量值序列之间的相关系数来实现变化缓变参数自动判读的方法.该方法对测量值序列进行先归一再累加生成的处理方式,克服了遥测系统测量误差对相关系数计算的影响,保障了判读准确性,同时减少了建立判读知识库的工作量.仿真结果表明,该方法运用简便,效果良好.     

Statistical characterisation of spread F over South Africa

The occurrence of mid-latitude spread F (SF) over South Africa has not been extensively studied since the installation of the DPS-4 digisondes in 1996 and 2000 at Grahamstown (33.32 °S, 26.50 °E) and Madimbo (22.38 °S, 30.88 °E) respectively. This study is intended to quantify the probability of occurrence of F region disturbances associated with SF over South Africa. A study was conducted using data for 8 years (2001–2008) over Madimbo (with a time resolution of 30 min) and Grahamstown (with a variable time resolution of 15 and 30 min). In this study, SF has been classified into frequency SF (FSF), range SF (RSF) and mixed SF (MSF). The SF events were identified by manually identifying ionograms showing SF and tabulating them according to type for further statistical analysis. The results show that the diurnal pattern of SF peaks strongly between 01:00 and 02:00 local time, LT (LT = UT + 2 h), where UT is the universal time. This pattern is true for all seasons and types of SF at Madimbo and Grahamstown in 2001 and 2005, except for RSF which had peaks during autumn and spring in 2001 at Madimbo. The probability of both MSF and FSF tends to increase with decreasing solar activity, with a peak in 2005 (a moderate solar activity period). The seasonal peaks of MSF and FSF are more frequent during winter months at both Madimbo and Grahamstown. In this study, SF was evident in ∼0.03% and ∼0.06% of the available ionograms at Madimbo and Grahamstown respectively during the 8 years.     

Rigidity spectrum of the 27-day variation of the galactic cosmic ray intensity in different epochs of solar activity

We study the temporal evolution of the power rigidity spectrum of the first (27 days) and the second (14 days) harmonics of the 27-day variation of the galactic cosmic ray intensity measured by neutron monitors in the period of 1965–2002. The rigidity spectrum of these variations can be approximated by a power law. We show the rigidity spectra of the first and the second harmonics of the 27-day variation of the galactic cosmic ray intensity have similar time profiles. These spectra are hard (γ ≈ 0.5 ± 0.1) and soft (γ ≈ 1.1 ± 0.2) during solar maximum and minimum activity, respectively. We ascribe this to the alternation of the sizes of the modulation regions responsible for the 27-day variation of the galactic cosmic ray intensity in different epochs of solar activity. Especially, the average radial sizes of the modulation regions of the 27-day variation and the heliolatitudinal extension of the heliolongitudinal asymmetry are smaller during solar minimum than during solar maximum. We show also, that the temporal changes of the power rigidity spectra of the first and the second harmonics of the 27-day variation of the galactic cosmic ray intensity are in a negative correlation with the changes of the rigidity spectrum of the corresponding 11-year variation.     

校罗差时磁偏差设定为零的机理分析

在飞机地面通常检查时,磁差给定器磁偏差值往往设定为当地磁差,才能得到正确的航向。校正磁罗差时,只有将磁差给定器设定为000.0,不然罗差计算会大大溢出指标。文章通过磁罗差校正的原理和校正方法的论述,进一步分析了校罗差时将磁偏给定器设定为000.0的工作机理。     

Latitudinal variation of the topside electron temperature at different levels of solar activity

A database of electron temperature (T_e) measurements comprising of most of the available satellite measurements in the topside ionosphere is used for studying the solar activity variations of the electron temperature T_e at different latitudes, altitudes, local times and seasons. The T_e data are grouped into three levels of solar activity (low, medium, high) at four altitude ranges, for day and night, and for equinox and solstices. We find that in general T_e changes with solar activity are small and comparable in magnitude with seasonal changes but much smaller than the changes with altitude, latitude, and from day to night. In all cases, except at low altitude during daytime, T_e increases with increasing solar activity. But this increase is not linear as assumed in most empirical T_e models but requires at least a parabolic approximation. At 550 km during daytime negative as well as positive correlation is found with solar activity. Our global data base allows to quantify the latitude range and seasonal conditions for which these correlations occur. A negative correlation with solar activity is found in the invdip latitude range from 20 to 55 degrees during equinox and from 20 degrees onward during winter. In the low latitude (20 to −20 degrees invdip) F-region there is almost no change with solar activity during solstice and a positive correlation during equinox. A positive correlation is also observed during summer from 30 degrees onward.