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   

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   

DInSAR技术对不同方位形变的敏感性研究   总被引：3，自引：1，他引：2  

查显杰  傅容珊  戴志阳 《测绘学报》2006,35(2):133-137

以DEM数据为假想的地面目标,只考虑距离对相位的影响,模拟竖直向、距离向和方位向形变的干涉纹图,从而研究DInSAR技术对空间不同方位形变的敏感性。在所有模拟参数和形变位移大小都相同的情况下,三个不同方位形变所产生的相位从0到2π变化的完整干涉环的数目是各不相同的,揭示DInSAR技术对不同方位地表形变的敏感性存在差异,且敏感性由大到小依次为:竖直向、距离向和方位向。  相似文献   

Mapping glacier velocities on Svalbard using ERS tandem DInSAR data     

《Norsk geografisk tidsskrift. Norwegian journal of geography》2012,66(4):276-285

The results presented show how glacier velocities can be measured and calculated from Earth Resources Satellite (ERS) tandem interferometric synthetic aperture radar (InSAR) data by the use of geographical information systems (GIS) and non-interferometric software. A semi-automatic algorithm using existing and newly implemented modules in ESRI's GIS software Arc has been developed to unwrap existing height differentiated interferometric SAR (DInSAR) data. The algorithm is applied to a data set covering glaciers from the arctic archipelago Svalbard. Estimated DInSAR velocities are decomposed into the glacier surface flow direction using a digital elevation model (DEM). Velocity fields for the glaciers Isachsenfonna, Akademikerbreen and Nordbreen on Svalbard are presented.  相似文献   

时间序列InSAR技术中的形变模型研究   总被引：1，自引：0，他引：1  

张永红  吴宏安  孙广通 《测绘学报》2012,41(6):864-869

时间序列InSAR技术,包括PS-InSAR技术和小基线集InSAR技术, 能有效克服传统D-InSAR的失相干限制, 逐步成为形变测量中的实用化技术。但是, 现有时间序列InSAR技术主要采用线性函数对真实形变进行模拟, 在真实形变呈现强烈的非线性时, 这种处理将不能得到正确的形变结果。本文就时间序列InSAR的形变模型问题展开研究, 首先从干涉相位模型解算的方法入手, 深入分析了线性形变模型的不足, 当干涉点目标的密度不够并且真实形变的非线性较强时, 干涉相位方程的解将会发散。根据魏尔斯特拉斯逼近定理, 提出以高阶多项式取代线性形变模型, 并给出了基于多项式形变模型的干涉相位方程解算方法。 利用太原市2003-2009年的23景ENVISAT ASAR影像, 分别采用线性形变模型和三次多项式形变模型, 利用小基线集技术进行了形变反演。将这两种方法得到的结果分别与水准测量结果进行了比较。结果表明, 采用多项式形变模型不仅能取得更高的形变测量精度,而且能提高点目标的密度。由于高阶多项式总能比低阶多项式更准确地拟合连续函数, 因此本文提出的多项式形变模型在时间序列InSAR形变监测中具有广泛的应用价值。  相似文献   

基于平面波模型重访地震背景噪声互相关及空间自相关(SPAC)     

鲁来玉 《地球与行星物理论评》2021,(2)

自Aki(1957)提出微震的空间自相关(SPatial AutoCorelation,SPAC)技术以来,SPAC技术一直独立发展,并在工程地震领域获得了广泛应用.近20年来,地震干涉(Seisimic Interferometry,SI)在多个领域引起人们的关注,该技术的核心思想是连续地震背景噪声的互相关函数(Noise Crosscorrelation Function,NCF)可以重建系统的格林函数(Green's Function,GF),对该技术的回溯性研究建立了SPAC和NCF的关系:它们是对同一物理现象的不同描述,SPAC在频率域中描述随机平稳噪声的空间相干,NCF在时间域中描述扩散场的互相关.理论上SAPC和NCF技术要求背景噪声源均匀分布,这样的噪声场可以用平面波叠加来模拟.本文基于平面波模型重访地震背景噪声的互相关和空间自相关技术,从单色平面波的互相关表示出发,对地震背景噪声互相关及空间自相关技术进行评述,试图使这些概念更易于理解.与之前众多研究地震干涉技术的理论相比,本文尤其关注以下几点:(1)基于简单的平面波模型,给出不同维度下,源或台站对方位均匀分布时,平面波互相关对入射波的方位平均和台阵对的方位平均结果,并对格林函数GF和时域互相关函数NCF的关系进行总结.(2)给出声源和(或)交叉台站方位分布不均匀时的互相关表示,指出这种非均匀性对方位的依赖关系,与弱各向异性介质中面波速度的方位依赖关系类似,因此,非均匀源的影响在反演时可能会映射到面波方位各向异性结果中.(3)互相关运算中,哪一个台站是虚拟源.NCF包含因果性和非因果性两部分,NCF的非对称性通常用于研究噪声源的方位分布,但由于源和接收的互易关系,及对互相关运算的不同定义和不同的傅里叶变换习惯,哪一个台站是虚拟源在目前的文献中并不明确.(4)方位平均和时间平均的关系.在SPAC处理中,需要对不同方位分布的台站对进行方位平均,本文从理论上说明,单个平面波入射时,交叉台站互相关系数对台站对的方位平均,等价于单个台站对互相关系数对入射波的时间平均.(5)几种特定分布非均匀噪声源的SPAC表示.包括单独的因果性噪声源和非因果性噪声源给出的互相关函数表示,及由此带来的相移问题.(6)利用SPAC、NCF和面波GF之间的关系,给出交叉分量的空间自相关系数表示.(7)衰减介质的空间相干表示.虽然利用地震干涉技术研究介质衰减在理论上仍然存在一些争议,但人们正试图研究从连续背景噪声记录中提取介质衰减的可能性.本文基于平面波模型,给出了不同坐标选择下,衰减介质的空间相干表示,这种表达的不同,指示了由地震干涉技术提取介质衰减的困难.与众多研究地震干涉的理论相比,比如稳相近似理论、互易定理、时间反转声学等,本文主要考虑均匀介质,不涉及非均匀介质的散射,从最简单的平面波模型,理解背景噪声重建系统格林函数这一地震干涉的核心思想和相应的基本概念.  相似文献   

Using the quasar VLBI network for the fundamental time—positioning service of the GLONASS space system     

A. M. Finkelstein  E. A. Skurikhina  I. F. Surkis  A. V. Ipatov  I. A. Rakhimov  S. G. Smolentsev 《Astronomy Letters》2008,34(1):59-68

Regular high-precision determinations of the Earth’s orientation parameters (EOPs) on the Quasar VLBI Network were begun in August 2006. The observations are performed within the framework of two national programs: daily sessions at three observatories of the Network to determine all five EOPs (the RU-E program) and 8-h sessions on the Zelenchukskaya-Badary and Svetloe-Badary baselines to determine the Universal Time (the RU-U program). The observations from August 2006 through May 2007 are analyzed. The rms deviations of the EOP values obtained in the RU-E program from the IERS C04 series are 1.1 mas for X _p and Y _p, 37 μs for UT1-UTC, and 0.7 and 0.6 mas for X _c and Y _c, respectively. These results closely match the prospective requirements of GLONASS. The rms deviations of the Universal Times obtained in the RU-U program from the IERS C04 series are 146 μs. We consider the immediate prospects for improving the accuracy of EOP determinations in daily sessions and for implementing the e-VLBI mode for an online determination of the Universal Time. Original Russian Text ? A.M. Finkelstein, E.A. Skurikhina, I.F. Surkis, A.V. Ipatov, I.A. Rakhimov, S.G. Smolentsev, 2008, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2008, Vol. 34, No. 1, pp. 66–76.  相似文献