A non-local vectorial total variational model for multichannel SAR image speckle suppression

This paper aims at the multichannel synthetic aperture radar(SAR)image speckle reduction.This paper proposes a novel energy minimized regularization model for multichannel image denoising,which is an extension of the non-local total variational model for gray-scale image.It contains two terms,namely the vectorial data fidelity term and the non-local vectorial total variation term.The latter is constructed by high-dimensional non-local gradient that contains the structure information of the multichannel image.The existence and the uniqueness of the solution of the model are proved.A fixed point iterative algorithm is designed to acquire the solution of this model.The convergence property of this algorithm is proved as well.This model is applied to the multipolarimetric and multi-temporal RADARSAT-2 images despeckling.The result shows that this model performs better than the original vectorial total variational model on texture preserving.     

基于2D-LDV技术的船舶螺旋桨三维流场结构分析(英文)

利用2D-LDV设备,通过优化布置测试点,获得了均匀来流下螺旋桨尾流场三维流动数据。展示了宏观的流场动态以及微观的流动信息,如尾涡和梢涡在流场中的分布情况、尾涡部流动的剪切效应、梢涡部的绕流及流动分离状态。计算了水动力螺距角以及螺旋桨附着涡的总环量。试验显示了LDV技术在流动细节测试方面的优势,获得的定量信息可以为相关研究人员提供技术支持。     

出口轮毂形状对大型轴流风机性能影响的数值研究

针对某大型轴流风机设计了4种出口段轮毂匹配方案,采用数值模拟方法对比分析了4种方案下的风机特性和叶尖以及叶根流场结构.结果表明:出口轮毂形状的变化对该风机叶尖流场结构影响很小;该风机出口无轮毂时,在叶根区域出现约占20%叶高区域的分离流,损失严重,降低了工作效率;在相同的叶尖间隙下,风机效率随着出口轮毂扩压角的减小而提高;在风机出口增加一个匹配的平直轮毂或收缩轮毂可使叶根分离涡后移,分离区域减小至5%叶高以下,同时可使该风机效率至少提高2个百分点.     

椭圆形切扇修形对波瓣混合器掺混性能影响

在保证面积不变的情况下,选取不同的长轴、短轴,对波瓣混合器进行椭圆形切扇修形,研究切口深度与宽度对波瓣混合器掺混性能的影响规律。使用商用 CFD 软件对流场进行数值模拟。结果显示,对波瓣侧壁进行切扇处理会加强流向涡的强度,切扇越深,流向涡强度越大;切扇波瓣流向涡的耗散速率要大于基准波瓣混合器的流向涡耗散速率,预示着更为高效的掺混;引射系数与切口深度成正比,而总压恢复系数与切口深度成反比。考察了两种衡量热混合效率的模型并对其信度进行了比较,发现在 x =0.4 m 之前切扇可以提高热混合效率,而在 x =0.4 m 之后,基准波瓣混合器热混合效率要大于切扇波瓣混合器。     

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.     

总体最小二乘算法在自适应信道均衡中的应用研究

分析了最小二乘解产生偏差的原因,推导出了最小二乘解偏差项的数学表达式。提出了一种基于瑞利商的变步长总体最小二乘求解方法。仿真试验表明,总体最小二乘算法的性能优于加权递归最小二乘算法,是一种适用于输入信号端含有噪声的自适应信道均衡算法。     

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.