PS-DInSAR公共主影像的优化选取   总被引：8，自引：1，他引：7  

陈强  丁晓利  刘国祥 《测绘学报》2007,36(4):395-399

在充分顾及DInSAR时空基线跨度及多普勒质心频率差异3个因素对干涉相关性影响的基础上,提出一种PS—DInSAR公共主影像的优化选取算法,采用综合相关测度作为总体干涉相关性的衡量指标,给出具体的综合相关函数模型及其求解方法。借助欧洲空间局（ESA）ERS-1／2卫星从1992—2002年间飞越上海地区所获取的25幅C波段SAR影像作为源数据,开展了PS—DInSAR公共主影像的优化选取实验。计算结果与分析表明,综合相关系数模型用于PS公共主影像的优化选取是有效的和可靠的。  相似文献   

TanDEM-X双站SAR干涉测量及研究进展     

孙亚飞  江利明  柳林  孙永玲  汪汉胜 《国土资源遥感》2015,(1)

较全面、系统地介绍了Tan DEM-X/Terra SAR-X双站SAR科学计划,重点涉及其科学目标、Tan DEM-X卫星参数、轨道结构以及干涉数据获取模式等相关内容,并讨论了双站SAR成像、极化In SAR和数字波束成形等干涉测量新技术及其研究进展。这些双站SAR新技术的实现将大大地推动SAR干涉测量在全球地形测绘、冰川学、海洋学及地质学等领域中的应用。  相似文献   

Attribution of Persistent Precipitation in the Yangtze–Huaihe River Basin during February 2019     

Zhixuan WANG  Jilin SUN  Jiancheng WU  Fangyue NING  Weiqi CHEN 《大气科学进展》2020,37(12):1389-1404

In February 2019, a month-long persistent precipitation event occurred in the Yangtze–Huaihe River basin. The geopotential height field that affected the duration of this frontal rainfall was divided into a high-latitude part and a low-latitude part for analysis. In the high-latitude part, a two-wave structure led to quasi-stationary circulation, and the change of both the blocking high pressure and Arctic Oscillation phase caused cold air to invade South China continuously and changed the frontal position. In mid-to-low latitudes, the persistent precipitation showed quasi-biweekly oscillation characteristics. The so-called “subtropical high–precipitation–anticyclone” (SHPA) feedback mechanism blocked the circulation systems in the mid-to-low latitudes and provided a continuous supply of water vapor for precipitation. As for the effect of sea surface temperature, the western North Pacific anomalous anticyclone stimulated by El Ni?o strengthened the intensity of the southerly wind and provided support for the redevelopment of the anticyclone system in the SHPA feedback mechanism. The sea surface temperature anomaly in the South China Sea provided sensible heating for precipitation, and convergent rising airflow was conducive to the occurrence of precipitation. Additionally, the SHPA mechanism provides a reliable basis for the prediction of persistent precipitation in winter in the mid-to-low latitudes.  相似文献   

2012年11月大气环流和天气分析     

黄威 《气象》2013,39(2):259-264

2012年11月环流特征如下:北半球极涡呈单极性分布,中心位于加拿大北部地区;欧亚中高纬环流经向度较大;南支槽平均位置大致位于90°E附近,且东移频繁;同时,副热带高压较常年同期偏强,位置偏西、偏北.11月,全国平均降水量为31.7 mm,比常年同期(18.8 mm)偏多68.6％.全国平均气温为2.0℃,比常年同期(2.9℃)偏低0.9℃.月内,出现4次全国范围中等强度冷空气过程和3次暴雨过程;华北、东北和内蒙古地区出现大范围强降雪和降温天气,其中华北大部地区出现今年冬半年首场降雪天气,京津地区、河北、内蒙古等地均出现极端降水;江南、华南出现持续阴雨寡照天气.  相似文献   

多回击负地闪先导通道的辐射和光学特征   总被引：1，自引：0，他引：1  

余海  张广庶  李亚珺  王彦辉  武斌  张荣  吕伟涛 《高原气象》2013,32(3)

利用闪电VHF窄带干涉仪辐射源定位系统和高速摄像系统,对青海大通地区一次有5次回击的负地闪放电过程进行了同步观测,对比分析了通道传输过程的辐射和光学特征.结果表明,光学通道亮度能补充VHF干涉仪定位先导通道的电流特征,VHF干涉仪定位弥补了光学设备拍摄弱放电和云内流光通道的不足;在通道分枝结构上,干涉仪定位的通道和光学通道呈现出很好对应.干涉仪定位分枝通道的辐射源点较明显,但分枝光学通道的出现明显落后于干涉仪定位辐射源通道.对用两种不同观测手段探测的先导通道进行速度计算,发现两者计算的直窜先导和直窜梯级先导速度量级一致,均为106m·s-1,但干涉仪在时间的获取及精确量化上有优势,干涉仪定位计算先导速度的精确度高于光学通道定位.  相似文献   

基于Voronoi图的强降水过程空间非均匀性定量表征方法     

彭小燕  杜银  丁裕国 《气象科技》2013,41(3):522-528

利用Voronoi\\Delaunay图模型影响范围和局部动态的特性,提出一种基于动态边界定量提取强降水过程空间非均匀分布特征的新方法,根据1959—2002年中国740站逐日降水资料,构建5日、10日两种时间尺度区域持续性年极端强降水过程序列,用以检验该方法的应用效果,并应用该方法分析了5日(10日)区域持续性年极端强降水过程空间非均匀分布特征及其演变规律。结果表明：与传统的数量统计方法和区域插值方法相比,该方法在强降水空间分布中心、过程内不同强度降水覆盖区域、降水集中区等的定量度量方面具有更高的分辨力和较好实际应用价值;气候趋势分析中在1959—2002年间,5日区域持续性年极端强降水过程出现日期有明显提前趋势。  相似文献   

Extragalactic Astronomy with the VLTI: a new window on the Universe     

Alessandro Marconi  Roberto Maiolino  Romain G. Petrov 《Astrophysics and Space Science》2003,286(1-2):245-254

Interferometry in the optical and near infrared has so far played a marginal role in Extragalactic Astronomy. Active Galactic Nuclei are the brightest and most compact extragalactic sources, nonetheless only a very limited number could be studied with speckle interferometry and none with long baseline interferometry. The VLTI will allow the study of moderately faint extragalactic objects with very high spatial resolution thus opening a new window on the universe. With this paper we focus on three scientific cases to show how AMBER and MIDI can be used to tackle open issues in extragalactic astronomy. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

The Wolf-Rayet stars at high (spatial) resolution     

A. Niedzielski 《Astrophysics and Space Science》2003,286(1-2):237-244

The Wolf-Rayet stars represent an advanced stage of evolution of the most massive stars. Their next immediate stadium will be supernova explosion. The most striking property of this very rare but exceptionally hot and bright objects is their extreme mass loss, of the order of 10^-5 solar mass per year. In turn of evolution before and during the Wolf-Rayet phase such stars eject a lot of matter (∼ 10 M_⊙) with velocity up to 3000 km/s that surrounds the min the form of gas and dust. In the case of binary Wolf-Rayet star such expanding envelope may interact with a companion (usually hot OB star) wind forming a tail extended for ∼ 100 AU. This spectacular phenomenon as well as some other connected with Wolf-Rayet stars that can be studied with high spatial resolution instruments (both astrometric and imaging) are reviewed. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

PRIMA for the VLTI – Science     

F. Delplancke  F. Derie  F. Paresce  A. Glindemann  F. Lévy  S. Lévêque  S. Ménardi 《Astrophysics and Space Science》2003,286(1-2):99-104

The four main scientific objectives of PRIMA – the Phase-Referenced Imaging and Micro-arc second Astrometry facility for the VLTI – will be described:– extra-solar system characterization with astrometry, to detect planets and evaluate their mass, and imaging of the dust accretion disk,– galactic center study with astrometry(dynamics of the bulge stars) and imaging at 10μm (piercing the gas and dust clouds surrounding the galactic center),– observations of AGNs and other extra-galactic objects, too faint to be observed without PRIMA, for which partial imaging is needed to constrain their structuremodels,– micro-gravitational lensing event resolution (imaging and astrometry of their photo-center) in the Galactic Bulge and Magellanic Clouds, helping to determine directly the lens mass and distance. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

Measuring the sizes of stars     

R. Hanbury Brown 《Journal of Astrophysics and Astronomy》1984,5(1):19-30

The Chatterton Astronomy Department aims to apply interferometers with very high resolving power to optical astronomy. The programme of the stellar intensity interferometer at Narrabri Observatory was completed in 1972 and since then the work has been directed towards building a more sensitive instrument with higher resolving power. As a first step a much larger intensity interferometer was designed but was not built because it was large, expensive and not as sensitive as desired. Efforts are now being made to design a more sensitive and cheaper instrument. A version of Michelson’s stellar interferometer is being built using modern techniques. It is hoped that it will reach stars of magnitude +8 and will work reliably in the presence of atmospheric scintillation. It is expected to cost considerably less than an intensity interferometer of comparable performance. The pilot model of this new instrument is almost complete and should be ready for test in 1984. Text of an Academy Lecture delivered at the Raman Research Institute, Bangalore on January 27, 1984.  相似文献