云闪放电通道发展及其辐射特征

利用闪电宽带干涉仪系统,对中国南方(广东)地区云闪时空演变特征、辐射及其相应电场变化特征进行分析研究。根据云闪电场变化波形,云闪放电过程可划分成活跃阶段和最后阶段,辐射源定位结果表明,云闪放电起始于向上发展的负击穿过程,通道向上发展的速度约为3～3.3×105m·s-1。云闪放电的主通道在活跃阶段形成,该期间辐射源随时间演变和相应电场变化表明,云内电荷结构具有上正下负的偶极性电荷结构。云闪的最后阶段辐射源主要在早期形成的通道内出现,其辐射源活动特征与地闪的回击过程比较相似;云闪辐射能量主要集中在2～3MHz以下的低频段,且辐射强度随频率增加迅速减弱。     

极化干涉SAR森林树高提取算法的对比分析

在对极化干涉SAR森林树高反演的DEM差值算法、相干相位-幅度综合反演算法进行分析的基础上,对基于极化干涉相干优化方法的改进算法进行了探讨。利用黑龙江大兴安岭地区的一对ALOS全极化干涉SAR数据进行实验,并对比分析各算法的反演结果。结果表明,在使用改进的算法进行森林树高反演时可以获取精度较高的反演结果,并且在一定程度上提高了森林树高反演的稳定性,为森林树高反演工作的业务化运行提供一定的依据。     

正交实验法在测绘中的应用

以检测数字水准仪及标尺综合精度为例，介绍了正交实验法在测绘领域中的应用。     

正交实验法在测绘仪器检定中的应用

在测绘生产和科研项目中，为了改革旧工艺或对新仪器，新产品,经常需要做多因素实验，如何安排多因素实验，是一个很值得研究的问题，文中以数字水准仪及标尺综合精度的检定为例，介绍了正交实验法在测绘仪器检定中的应用。     

河外射电源的结合阵数据的图像处理

不同类型的射电望远镜阵的分辨率差异甚大，用它们的数据进行图像处理后所得到的源结构的尺度也不一样。为了得到中间尺度的结构信息，有时我们需要把不同类型的射电望远镜阵的观测数据结合起来再进行图像处理。本文阐述我们把不同类型阵的数据结合时所用的方法；也给出我们使用的方法所获得的结果的实际例子。     

数字水准仪与精密光学水准仪测量精度比较

数字水准仪的出现解决了大地测量仪器中水准仪自动读数与记录问题,对当代测量技术产生了积极的影响.文中介绍了如何采用双频激光干涉仪配合45°平面镜检测数字水准仪的方法,对精密光学水准仪和数字水准仪进行综合精度的评定和比较,并对结果进行了分析.     

数字水准仪与精密光学水准仪测量精度比较

数字水准仪的出现解决了大地测量仪器中水准仪自动读数与记录问题,对当代测量技术产生了积极的影响。文中介绍了如何采用双频激光干涉仪配合45°平面镜检测数字水准仪的方法,对精密光学水准仪和数字水准仪进行综合精度的评定和比较,并对结果进行了分析。     

基于干涉仪原理的甚高频雷电单站预警

针对目前闪电单站探测与预警装置的局限性,设计了一套基于闪电宽带干涉仪原理的甚高频单站雷电预警装置.该装置通过测量雷电(包括云闪与地闪)起始时刻的辐射信号到达竖直天线阵列的相位差,计算得到该信号的仰角,根据仰角估算雷电的距离,进而根据雷电的距离和活动特征进行雷电报警.单站测距误差分析结果表明,单站系统对半径50 km范围内闪电测距误差在25％以内,半径100 km范围内的闪电测距误差在30％以内.雷电单站预警装置对一次雷暴过程进行了观测,观测结果表明,该装置能有效探测半径100 km范围内的闪电活动状况,探测到的闪电频次分布、闪电距离与多站闪电定位结果保持较好一致性,证明其能有效探测周围闪电活动状况,起到提前预警雷暴的作用.     

Gaseous Jets in Comet Hale-Bopp (1995 O1)

We report the identification of gas jets in comet Hale-Bopp in OH, NH, CN, C₂ and C₃. This is the first time OH and NH jets without an obvious optical dust jet counterpart have been identified in narrowband comet images. We also confirm the existence of CN jets as reported by Larson et al. (1997) and Mueller et al. (1998). Jet features can be seen in the March and April 1997 datasets, approximately a month before and after perihelion. Our results contribute to the understanding of both the chemical properties of the comet as well as the physical mechanisms necessary to produce these features. This revised version was published online in July 2006 with corrections to the Cover Date.     

Luciola hypertelescope space observatory: versatile, upgradable high-resolution imaging, from stars to deep-field cosmology

Luciola is a large (1 km) “multi-aperture densified-pupil imaging interferometer”, or “hypertelescope” employing many small apertures, rather than a few large ones, for obtaining direct snapshot images with a high information content. A diluted collector mirror, deployed in space as a flotilla of small mirrors, focuses a sky image which is exploited by several beam-combiner spaceships. Each contains a “pupil densifier” micro-lens array to avoid the diffractive spread and image attenuation caused by the small sub-apertures. The elucidation of hypertelescope imaging properties during the last decade has shown that many small apertures tend to be far more efficient, regarding the science yield, than a few large ones providing a comparable collecting area. For similar underlying physical reasons, radio-astronomy has also evolved in the direction of many-antenna systems such as the proposed Low Frequency Array having “hundreds of thousands of individual receivers”. With its high limiting magnitude, reaching the m _v?=?30 limit of HST when 100 collectors of 25 cm will match its collecting area, high-resolution direct imaging in multiple channels, broad spectral coverage from the 1,200 Å ultra-violet to the 20 μm infra-red, apodization, coronagraphic and spectroscopic capabilities, the proposed hypertelescope observatory addresses very broad and innovative science covering different areas of ESA’s Cosmic Vision program. In the initial phase, a focal spacecraft covering the UV to near IR spectral range of EMCCD photon-counting cameras (currently 200 to 1,000 nm), will image details on the surface of many stars, as well as their environment, including multiple stars and clusters. Spectra will be obtained for each resel. It will also image neutron star, black-hole and micro-quasar candidates, as well as active galactic nuclei, quasars, gravitational lenses, and other Cosmic Vision targets observable with the initial modest crowding limit. With subsequent upgrade missions, the spectral coverage can be extended from 120 nm to 20 μm, using four detectors carried by two to four focal spacecraft. The number of collector mirrors in the flotilla can also be increased from 12 to 100 and possibly 1,000. The imaging and spectroscopy of habitable exoplanets in the mid infra-red then becomes feasible once the collecting area reaches 6 m², using a specialized mid infra-red focal spacecraft. Calculations (Boccaletti et al., Icarus 145, 628–636, 2000) have shown that hypertelescope coronagraphy has unequalled sensitivity for detecting, at mid infra-red wavelengths, faint exoplanets within the exo-zodiacal glare. Later upgrades will enable the more difficult imaging and spectroscopy of these faint objects at visible wavelengths, using refined techniques of adaptive coronagraphy (Labeyrie and Le Coroller 2004). Together, the infra-red and visible spectral data carry rich information on the possible presence of life. The close environment of the central black-hole in the Milky Way will be imageable with unprecedented detail in the near infra-red. Cosmological imaging of remote galaxies at the limit of the known universe is also expected, from the ultra-violet to the near infra-red, following the first upgrade, and with greatly increasing sensitivity through successive upgrades. These areas will indeed greatly benefit from the upgrades, in terms of dynamic range, limiting complexity of the objects to be imaged, size of the elementary “Direct Imaging Field”, and limiting magnitude, approaching that of an 8-m space telescope when 1,000 apertures of 25 cm are installed. Similar gains will occur for addressing fundamental problems in physics and cosmology, particularly when observing neutron stars and black holes, single or binary, including the giant black holes, with accretion disks and jets, in active galactic nuclei beyond the Milky Way. Gravitational lensing and micro-lensing patterns, including time-variable patterns and perhaps millisecond lensing flashes which may be beamed by diffraction from sub-stellar masses at sub-parsec distances (Labeyrie, Astron Astrophys 284, 689, 1994), will also be observable initially in the favourable cases, and upgrades will greatly improve the number of observable objects. The observability of gravitational waves emitted by binary lensing masses, in the form of modulated lensing patterns, is a debated issue (Ragazzoni et al., MNRAS 345, 100–110, 2003) but will also become addressable observationally. The technology readiness of Luciola approaches levels where low-orbit testing and stepwise implementation will become feasible in the 2015–2025 time frame. For the following decades beyond 2020, once accurate formation flying techniques will be mastered, much larger hypertelescopes such as the proposed 100 km Exo-Earth Imager and the 100,000 km Neutron Star Imager should also become feasible. Luciola is therefore also seen as a precursor toward such very powerful instruments.