基于光谱知识库对高光谱影像目标快速识别方法

针对国内引进的机载高光谱成像仪（CASI/SASI）数据采集系统,介绍了利用先验知识建立的多种地物目标光谱库,以及高光谱影像目标快速识别的技术方法研究;同时还阐述了其数据处理流程、目标识别原理和应用开源代码编程实现过程,并对其结果与应用进行了简要的分析。     

地震成像技术在松辽盆地北部深层的应用研究

松辽盆地北部某地区深部地层倾角较陡,地下构造复杂,以叠加为基础的叠后时间偏移成像模糊。通过对深层复杂地质叠前时间偏移成像关键技术的研究,提出了综合建模静校正方法,以克服处理中出现的长波长静校正问题及连片处理中闭合差问题,并有针对性地采用了叠前噪声压制技术、球面扩散补偿、地表一致性振幅补偿及剩余振幅补偿技术、多域统计地表一致性反褶积技术和Kirchhoff叠前偏移算法。结果表明,采用上述组合地震数据处理技术,可有效提高松辽北部深层复杂地质体的偏移成像质量,为准确识别其火山岩储层和火山岩气藏圈闭提供可靠的技术支撑。     

测井方法在观测采空区上覆岩层导水裂隙带发育高度中的应用

新安矿区主采煤层上部至小浪底库区水体之间地层主要以砂岩、泥岩和砂质泥岩互层为主,厚度90~210m。为研究该矿开采状态下上覆岩层破坏程度和导水裂隙发育高度,在井下3个不同采厚的工作面上布置了7个地面钻孔,采用声波扫描成像测井及其它测井参数对采前、采后上覆岩层进行动态观测。以K3钻孔为例,介绍了超声波扫描成像测井的原理及辨别井孔中裂缝发育程度的方法。K3孔在第一次测量时,井深217～218m处明显存在裂隙,但在第二次测量后该裂隙呈现出闭合反应,证实煤层开采放顶后上部岩石下沉使得原有裂隙闭合;同时发现自194m以上因煤层采空放顶后发育有高度为69.10m的裂隙带。根据新安煤矿K2、K3、K5、K6、K7号孔超声波扫描成像及其它常规测井的地质解释成果可见,该矿导水裂隙带的发育高度随着推进距离和采厚增大而增大,但新安矿区软硬互层上覆岩层的地质构造可有效抑制导水裂隙带的发育程度。     

Numerical investigation of wave propagation in the Liverpool Bay, NW England

The computer model for near shore wave propagation,SWAN,was used to study wave climates in Liverpool Bay,northwest England with various input parameters,including bottom friction factor,white capping,wind drag formulation and effects of tidal modulations.Results were compared with in-situ measurements and reveal the impacts from these inputs on the predictions of wave height and propagation distributions.In particular,the model results were found very sensitive to different input formulations,and tend to underestimate the wave parameters under storm conditions in comparison with the observations.It is therefore important to further validate the model against detailed field measurements,particularly under large storms that are often of the primary concern.     

The ultrastructure of the spermatozoon of Octopus ocellatus Gray, 1849 (Cephalopoda: Octopoda)

Morphology of the spermatozoon of Octopus ocellatus was studied by light, scanning electron, and transmission electron microscopes. Sperm are 600–700 μm long, with a large number of granules in diameter about 130 nm. Each spermatozoon is composed of a head, neck, and tail. The head is made up of an acrosomal complex anterior to the nucleus. The spiral acrosomal complex consists of an electron-lucent vesicle, lacuna, and an electron-dense acrosomal vesicle. Additionally, the spiral acrosomal vesicle has numerous equidistant striations, and is surrounded by many small granules (20 nm diameter). A long straight nucleus, which is electron-densed, has a deep posterior concavity, the nuclear vacuole. At the terminal end of the nucleus is a sleeve-like structure with a concave posterior nuclear fossa (PNF). The neck is short connecting the PNF. The basal body is located in the PNF and gives rise to the axoneme. This structure connects the head, neck, and tail. The tail is divided into a middle piece and a principal piece. The middle piece, having a 9+9+2 arrangement, is surrounded by a mitochondrial sheath and terminates by an electron-dense fibrous sheath. The principal piece is the longest part of the sperm with coarse fibers tapering posteriorly. The results of this study shall provide some useful information for artificial breeding of this species.     

A polarimetric spectral imager using acousto-optic tunable filters

We report laboratory and telescopic observations with a polarimetric spectral imager based on an acousto-optic tunable filter (AOTF) where we demonstrate simultaneous acquisition of orthogonally polarized images at a spectral resolving power on the order of 103 and at a Rayleigh criterion spatial resolution of 100 line pairs per mm. This matches the spatial resolution of most digital arrays. An AOTF is shown to be usable as a fast shutter with a contrast of over 10⁴ on a sub-millisecond time scale while providing an high transmittance of about 75% (both polarizations summed) when illuminated by white light. The polarization contrast between the orthogonally polarized images exceeds 10⁴ across the field of view, permitting accurate measurement of the polarization parameters of incident light. These characteristics are now being used in a program of high spatial resolution imaging in narrow spectral bands. Some peculiarities and limitations of AOTFs are indicated.This research was supported by NASA under Grant NAGW-122 and under contract with the Jet Propulsion Laboratory under NASA grant NAS 7-918.Visiting Astronomer, Mauna Kea Observatory.     

The VLTI – A Status Report

The Very Large Telescope (VLT) Observatory on Cerro Paranal (2635 m) in Northern Chile is approaching completion. After the four 8-m Unit Telescopes (UT) individually saw first light in the last years, two of them were combined for the first time on October 30, 2001 to form a stellar interferometer, the VLT Interferometer. The combination in pairs of all four UTs was completed in September 2002. In this article, we will describe the subsystems of the VLTI and the planning for the following years. This revised version was published online in July 2006 with corrections to the Cover Date.     

Hemispheric Imaging of Galactic Neutral Hydrogen with a Phased Array Antenna System

The thousand element array (THEA) system is a phased array system consisting of 1 m² tiles having 64 Vivaldi elements each, arranged on a regular 8-by-8 grid, which has been developed as a demonstrator of technology and applicability for SKA. In this paper we present imaging results of Galactic neutral hydrogen with THEA. Measurements have been taken using a dense 2-by-2 array of four tiles as a four tile adder. The results are compared with results from the Leiden-Dwingeloo Survey, showing qualitative agreement, but also indicating that further studies are needed on the instrumental characteristics.