Imaging Borrelly     

L.A Soderblom  D.C Boice  R.H Brown  R.L Kirk  R.M Nelson  B.R Sandel  N Thomas 《Icarus》2004,167(1):4-15

The nucleus, coma, and dust jets of short-period Comet 19P/Borrelly were imaged from the Deep Space 1 spacecraft during its close flyby in September 2001. A prominent jet dominated the near-nucleus coma and emanated roughly normal to the long axis of nucleus from a broad central cavity. We show it to have remained fixed in position for more than 34 hr, much longer than the 26-hr rotation period. This confirms earlier suggestions that it is co-aligned with the rotation axis. From a combination of fitting the nucleus light curve from approach images and the nucleus' orientation from stereo images at encounter, we conclude that the sense of rotation is right-handed around the main jet vector. The inferred rotation pole is approximately perpendicular to the long axis of the nucleus, consistent with a simple rotational state. Lacking an existing IAU comet-specific convention but applying a convention provisionally adopted for asteroids, we label this the north pole. This places the sub-solar latitude at ∼60° N at the time of the perihelion with the north pole in constant sunlight and thus receiving maximum average insolation.  相似文献   

Surveying co-located space-geodetic instruments for ITRF computation   总被引：2，自引：2，他引：0  

P.?SartiEmail author  P.?Sillard  L.?Vittuari 《Journal of Geodesy》2004,78(3):210-222

A new and comprehensive method is presented that can be used for estimating eccentricity vectors between global positioning system (GPS) antennas, doppler orbitography and radiopositioning integrated by satellites (DORIS) antennas, azimuth-elevation (AZ-EL) very long baseline interferometry (VLBI) telescopes, and satellite laser ranging (SLR) and lunar laser ranging (LLR) telescopes. The problem of reference point (RP) definition for these space-geodetic instruments is addressed and computed using terrestrial triangulation and electronic distance measurement (EDM) trilateration. The practical ground operations, the surveying approach and the terrestrial data processing are briefly illustrated, and the post-processing procedure is discussed. It is a geometrically based analytical approach that allows computation of RPs along with a rigorous statistical treatment of measurements. The tight connection between the geometrical model and the surveying procedure is emphasized. The computation of the eccentricity vector and the associated variance–covariance matrix between an AZ-EL VLBI telescope (with or without intersecting axes) and a GPS choke ring antenna is concentrated upon, since these are fundamental for computing the International Terrestrial Reference Frame (ITRF). An extension to RP computation and eccentricity vectors involving DORIS, SLR and LLR techniques is also presented. Numerical examples of the quality that can be reached using the authors approach are given. Working data sets were acquired in the years 2001 and 2002 at the radioastronomical observatory of Medicina (Italy), and have been used to estimate two VLBI-GPS eccentricity vectors and the corresponding SINEX files.  相似文献   

无控制DEM表面差异探测研究   总被引：1，自引：1，他引：0  

张同刚  岑敏仪  吴兴华 《测绘科学》2006,31(3):36-38

本文提出了一个新的无控制DEM差异探测算法。它可以将不同时期获取的DEM纳入到统一坐标系中,这样就可以根据匹配后的DEM来定量探测地表变化情况。该方法通过差分模型考虑了观测量的数值及其相互关系。与目前差异探测能力最强的LMS-LZD方法相比,新方法具有更好的差异能力和更高的匹配精度。普歪沟泥石流沟多时相DEM差异探测实例验证了新方法的优越性。  相似文献   

遗传算法优化的支持向量机湿地遥感分类——以洪河国家级自然保护区为例   总被引：6，自引：1，他引：5  

臧淑英  张策  张丽娟  张玉红 《地理科学》2012,(4):434-441

湿地遥感分类作为湿地管理、监测与评价的重要手段,受到了广泛的关注。遗传算法(GA)借鉴了生物进化规律进行启发式搜索寻优,支持向量机(SVM)是一种新型的空间数据挖掘方法,二者相结合可以发挥各自的优势,寻找到支持向量机的全局最优参数,从而较准确地对湿地进行遥感分类。以洪河自然保护区为例,采用遗传算法优化的支持向量机方法进行了湿地遥感分类研究。同格网搜索下的支持向量机湿地遥感分类及最大似然监督分类对比,结果表明,遗传算法优化较格网搜索方式总精度提高了7.29%,较最大似然监督分类提高了12.06%,方法改善了沼泽、草地与裸地三种地物间的区分,是湿地遥感分类的有效手段。  相似文献   

S波段双线偏振雷达KDP参数计算的初步研究          下载免费PDF全文

胡鹏  胡明宝  张柽柽  杨金伟 《气象与环境学报》2012,28(1):77-81

双线偏振多普勒雷达测量的参数K_DP在定量估测降雨强度和识别降水粒子相态方面都有着很重要的作用。鉴于雷达实测K_DP值来源于S波段双线偏振雷达信号处理器（RVP8）的结果,没有具体的计算过程,不便于进行雷达资料预处理和质量控制。探讨总结了K_DP的3种算法,通过实测数据,将雷达信号处理器（RVP8）观测的K_DP作为参考值,进行了对比分析。结果表明：最小二乘法误差最小,精度最高;讨论了沿雷达径向,不同平滑距离对最小二乘法K_DP计算的影响;同时研究了雷达实测K_DP与通过Z-R关系计算的降雨强度之间的关系显示,5 km的距离长度既能起到足够的平滑作用,又能保持足够的气象信息,不至于影响测量降水效果;同时,K_DP与降雨强度之间存在较好的对应关系,在强降雨阶段尤为显著,可以利用K_DP来估算反演降雨强度。  相似文献   

重庆电网GIS平台建设     

白云庆  聂静  陈珏  李振  陈颋 《测绘信息与工程》2012,37(5):73-75

重庆电网GIS平台运用国产软件搭建网省信息化平台,完成了数据准备、软硬件环境、平台实施部署、应用系统集成等内容,该文介绍了其主要功能和关键技术。  相似文献   

Space charge generation in the atmosphere and the density of mechanical transfer current to the ground     

I.N. Panchishkina  G.G. Petrova  A.I. Petrov  T.V. Kudrinskaja 《Atmospheric Research》2009,91(2-4):238-243

The correlation of mechanical transfer current from the atmosphere to the ground with the process of space charge formation as a result of conductivity current divergence near ground is under discussion in this research. Experimental data of conductivity current and mechanical transfer current acquired at three observation points for different meteorological conditions are analyzed. In particular, the peculiarities of mechanical charge transfer to ground under different stratifications of the surface layer are under discussion.  相似文献   

Io's dayside SO₂ atmosphere     

Lori M. Feaga  Melissa McGrath 《Icarus》2009,201(2):570-1189

An extensive set of HI Lyman-α images obtained with the Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) from 1997-2001 has been analyzed to provide information about the spatial and temporal character of Io's SO₂ atmosphere. An atmospheric distribution map derived from the observations reveals that the sunlit SO₂ atmosphere is temporally stable on a global scale, with only small local changes. An anti-/sub-jovian asymmetry in the SO₂ distribution is present in all 5 years of the observations. The average daytime atmosphere is densest on the anti-jovian hemisphere in the equatorial regions, with a maximum equatorial column density of 5.0×¹⁰¹⁶ cm−2 at 140° longitude. The SO₂ atmosphere also has greater latitudinal extent on the anti-jovian hemisphere as compared to the sub-jovian. The atmospheric distribution appears to be best correlated with the location of hot spots and known volcanic plumes, although small number statistics for the plumes limits the correlation.  相似文献   

The C1XS X-ray Spectrometer on Chandrayaan-1   总被引：1，自引：0，他引：1  

M. Grande  B.J. Maddison  B.J. Kellett  J. Huovelin  C.L. Duston  M. Anand  A. Cook  B. Foing  J.N. Goswami  K.H. Joy  D. Kochney  S. Maurice  S. Narendranath  D. Rothery  A. Shrivastava  M. Wilding 《Planetary and Space Science》2009,57(7):717-724

The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray spectrometer for the Indian Space Research Organisation (ISRO) Chandrayaan-1 lunar mission. It exploits heritage from the D-CIXS instrument on ESA's SMART-1 mission. As a result of detailed developments to all aspects of the design, its performance as measured in the laboratory greatly surpasses that of D-CIXS. In comparison with SMART-1, Chandrayaan-1 is a science-oriented rather than a technology mission, leading to far more favourable conditions for science measurements. C1XS is designed to measure absolute and relative abundances of major rock-forming elements (principally Mg, Al, Si, Ca and Fe) in the lunar crust with spatial resolution ?25 FWHM km, and to achieve relative elemental abundances of better than 10%.  相似文献   

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

Antoine Labeyrie  Hervé Le Coroller  Julien Dejonghe  Olivier Lardière  Claude Aime  Kjetil Dohlen  Denis Mourard  Richard Lyon  Kenneth G. Carpenter 《Experimental Astronomy》2009,23(1):463-490

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.  相似文献