X波段双线极化雷达反射率的衰减订正

X波段雷达虽然其衰减较S和C波段雷达严重, 但是由于其易于移动等特点, 还在各国推广应用, 为了反演获得可靠的降水分布, X波段雷达数据需要进行衰减订正。本文提出一种基于气象目标和单位差分传播相移KDP特性的衰减订正方法。KDP由前向和后向两个分量组成, 为了计算KDP, 必须分离这两个分量以及消除其他随机噪声的影响。本文引进了一种最优化自回归数据滤波算法——卡尔曼滤波来分离这两个分量和消除其他随机噪声。这种方法效率高、实用性强, 同时可以用于其他雷达信号的处理。比较衰减订正结果, 发现使用卡尔曼滤波方法处理后的差分传播相移所进行的反射率衰减订正具有较高的稳定性。     

合肥上空卷云和沙尘气溶胶退偏振比的激光雷达探测

研制了一台L300偏振激光雷达,用于卷云和沙尘气溶胶后向散射光退偏振比的探测研究.介绍了偏振激光雷达的探测原理,叙述了L300偏振激光雷达的结构、技术参数、测量方法和数据处理方法.初步的探测结果表明,合肥西郊上空高度在10 km左右的卷云的退偏振比在0.4～0.5之间,沙尘气溶胶的退偏振比在0.2～0.3范围内,但是剧烈沙尘暴的气溶胶的退偏振比可达到0.4左右.     

新疆巴楚-伽师6.8级地震序列震源特征的初步研究

利用喀什国家数字地震台记录的巴楚—伽师6．8级地震序列资料,通过恢复震源位移谱,跟踪分析了序列中3级以上地震的应力降,同时与1997年强震群结果进行对比,讨论了本次地震的应力释放情况。分析结果表明：本次6．8级地震序列与1997年强震群序列相比,地震的应力释放为高应力释放,地震发展成为强震群型的可能性较小。还结合S波偏振分析方法尝试判断了震区几次5级以上地震震源机制的相对变化以及目前的应力状态。     

利用相控阵及双偏振雷达对2016年6月3日华南一次强对流过程的分析

本文结合X波段相控阵雷达(XPAR)和S波段双偏振天气雷达(SPOL)及地面和探空观测资料,分析了2016年6月3日发生在华南的一次超级单体中小尺度特征,结果表明:(1)SPOL的多普勒参量和双偏振参量可以观测到超级单体的强度、速度和相态分布,超级单体的入流和出流影响钩状回波的形成。(2)XPAR可以获取时空分辨率远高于SPOL的观测资料,可以弥补SPOL仰角层严重不足的缺陷,观测到超级单体完整的垂直结构,可更精确地描述超级单体的短时演变。(3)超级单体钩状回波附近给地面带来了降温、大风和强降水,超级单体经过地区均有明显降温和风区。研究结果证明相控阵雷达和双偏振雷达对认识对流单体中小尺度系统的发展演变有较大帮助。     

VLBI polarization images of eight compact active galactic nuclei at λ = 1.3 cm

Global VLBI images in intensity and linear polarization at     of the BL Lacertae objects 0235+164, 0300+470, 0735+178, 0954+658, 1803+784, 1823+568, and BL Lac and OVV quasar 3C 279 are presented and analysed. These are the highest resolution polarization images currently available for several of these sources. On the whole, the tendencies observed at longer centimetre wavelengths are also exhibited in these 1.3-cm images. When core polarization is detected, the corresponding polarization angles χ tend to lie either parallel or perpendicular to the direction of the inner jet. The core degrees of polarization are usually comparable to those typical at 6 cm, but somewhat lower in several cases, suggesting that the higher resolution data are better separating the contributions of intrinsically weakly polarized cores and highly polarized emerging knots. The observed χ vectors in the jets of 0735+178, 0954+658, 1823+568, BL Lac and 3C 279 are aligned with the jet, implying the presence of transverse magnetic fields. In 0300+470 and BL Lac, there are regions where the direction of χ seems to be neither parallel nor perpendicular to the jet; it is not clear whether this is due to genuine obliquity of the magnetic field structure or to inadequate knowledge of the local flow direction.     

The Self-Inversion of the Sign of Circular Polarization in “Halo” Microwave Sources

The large active region AR NOAA 5200 from October 1988 is used to investigate the concept of the “halo,” a magnetosphere-like structure above the active region. This structure is studied by using radio spectral polarization observations with high spatial resolution obtained mainly with the radio telescope RATAN-600. In the case of AR 5200 the halo emission accounted for >50% of the total AR emission. The results of the analysis of the observational data and of the model calculations allow us to reach the following conclusions: (1) The halo is a large, nonstructured, source of emission with a size of the total AR, with the emission centered at the dividing (neutral) line of polarities of the bipolar sunspot group. (2) The emission spectrum allows us to distinguish two components: a thermal part and a nonthermal part. The presence of two components implies that there are two populations of particles with different energy levels in the emission region. The phenomenon of inversion of the polarized halo radio emission could be explained by the influence of propagation conditions inside the source. The term “self-inversion” is introduced. The maximum in the halo density flux spectrum at wavelengths of 5 –10 cm may be explained by scattering resulting from the strong suppression of the emissivity of nonthermal electrons at these and longer wavelengths.     

An Intrinsic Model for the Polarization Position Angle Swing Observed in QSO 1150＋812

The rapid polarization position angle swing of ~ 180?observed in QSO 1150+812 at 2cm by Kochenov and Gabuzda is quite a regular event. One interesting property of the event is that, during the time of the swing the polarized flux density remained almost constant. We suggest that such an event can be explained in terms of a relativistic thin shock propagating through a uniform helical magnetic field, giving rise to relativistic aberration effects as the transverse field component rotates. The model may also be applicable to other similar events in which variations in polarization are not accompanied by variations in total flux density.     

基于正交偏光序列消光特征的岩石薄片颗粒分割与孔隙提取

在岩石薄片正交偏光显微镜下角度域序列图像采集的基础上,分析了不同岩石组分在消光角度域上的光学特征及其差异性,并据此提出一种新的岩石颗粒分割和孔隙分析的方法。充分利用岩石颗粒赋存状态及其晶体光轴产状的复杂性、岩石颗粒空间排列及其接触关系的多样性,对岩石薄片在消光角维度上进行像素尺度的相关分析,并提出相关系数均值、相关系数标准差以及相关系数均差比等敏感参数,实现了岩石颗粒的分割和孔隙的提取。研究表明岩石颗粒内部的像素点灰度和RGB值在角度域上的相关性较强,在颗粒边缘及孔隙内部填隙物分布区域,其相关系数较低,且相关系数标准差要明显高于岩石颗粒内部。该方法从消光特征出发论证了角度域信息完整性的意义,提取的颗粒边缘较为清晰,孔隙结构骨架得以刻画,颗粒分割的效果好于Sobel和Canny等方法。