基于Flex和.NET的B/S系统权限管理的设计与实现

RIA技术具有交互能力强、界面表现力丰富等特点,成为目前B/S系统的主要开发方式。而权限管理作为系统必不可少的组成部分,是系统稳定和数据安全的保障。介绍开发过程中使用的主要技术,阐述基于Flex和.NET技术开发的权限管理的设计方案和实现方法,并成功应用于工业总图共享服务系统中。实践证明,该权限管理设计方案具有灵活简便、安全性高、扩展性强和业务无关性等优点。     

TRMM3B42降水产品在鄱阳湖流域梅川江子流域的精度评价(英文)

在鄱阳湖流域的梅川江子流域,利用52个站点9年(2001-2005及2007-2010)的日降水数据对V6和V7两个版本的TRMM 3B42降水产品进行了精度评价。该评价针对多个时空尺度进行,包括栅格和流域两个空间尺度,日、月和年三个时间尺度。为避免尺度不匹配问题,本文利用泰森多边形方法将点尺度的站点观测数据转换到与TRMM数据相同的栅格尺度。评价结果表明,V6和V7两个版本的TRMM3B42降水产品差别较小,整体上均轻微高估了降水量(偏差均为0.04)。在日尺度,栅格和流域空间尺度上V6和V7TRMM3B42降水产品的精度均较差,相对均方根误差在135%-199%之间。因此,在该地区利用3B42数据进行日尺度的水文分析前需要对其进行校正。在月和年尺度,栅格和流域两个空间尺度上V6和V7两个版本的TRMM 3B42降水产品精度均较高,决定系数达到0.91-0.99,相对均方根误差在4%-23%之间。这表明TRMM 3B42降水产品在该地区月和年尺度的水文分析方面具有很好的应用前景。     

X-ray observations of PSR B1259−63 near the 2007 periastron passage

PSR B1259−63 is a 48-ms radio pulsar in a highly eccentric 3.4-yr orbit with a Be star SS 2883. Unpulsed γ-ray, X-ray and radio emission components are observed from the binary system. It is likely that the collision of the pulsar wind with the anisotropic wind of the Be star plays a crucial role in the generation of the observed non-thermal emission. The 2007 periastron passage was observed in unprecedented details with Suzaku , Swift , XMM–Newton and Chandra missions. We present here the results of this campaign and compare them with previous observations. With these data we are able, for the first time, to study the details of the spectral evolution of the source over a 2-month period of the passage of the pulsar close to the Be star. New data confirm the pre-periastron spectral hardening, with the photon index reaching a value smaller than 1.5, observed during a local flux minimum. If the observed X-ray emission is due to the inverse Compton (IC) losses of the 10-MeV electrons, then such a hard spectrum can be a result of Coulomb losses, or can be related to the existence of the low-energy cut-off in the electron spectrum. Alternatively, if the X-ray emission is a synchrotron emission of very high-energy electrons, the observed hard spectrum can be explained if the high-energy electrons are cooled by IC emission in Klein–Nishina regime. Unfortunately, the lack of simultaneous data in the TeV energy band prevents us from making a definite conclusion on the nature of the observed spectral hardening and, therefore, on the origin of the X-ray emission.     

基于B／S（Browser／Server）架构的深圳市交通预报制作系统的设计与实现

2005年7月27日中国气象局和交通部联合签署了《共同开展公路交通气象监测预报预警工作备忘录》。随着该《备忘录》的签署,深圳市气象局积极响应,着手研究交通天气预报技术和方法,并于2006年9月28日正式开展了深圳市长途交通专题天气预报。为了达到交通预报制作图文并茂且节省人力的目的,采用B/S(Browser/Server)架构,对原C/S结构的交通预报制作系统进行了改进和升级,该系统使用PHP语言作为开发语言,并使用MYSQL作为数据库驱动。升级后的系统平台具有简洁、易于操作、安全性高、自动化程度较高和维护和升级简单的特点。     

ZK框架在开发基于B/S结构的气象信息共享发布系统中的应用

Ajax作为改进传统B/S结构应用系统的RIA模式的方案之一,在大量企业应用中被使用,如Google Maps等.ZK是实现Ajax的技术框架之一,具有简单易用、界面美观、交互丰富的优势.针对气象部门丰富的信息资源需要共享、发布的需求,介绍ZK框架在气象信息共享发布系统开发中的应用要点.     

差示FT-Raman和11B NMR方法研究过饱和镁硼酸盐的溶液结构

用差示FT -Raman和11BNMR光谱研究了MgB6O10 ·7 5H2 O、MgB4O7·9H2 O、Mg2 B6O10 ·1 5H2 O三种镁硼酸盐饱和和过饱和溶液的结构机理 ,其结果表明饱和溶液和过饱和溶液中均存在B(OH) 3 、B(OH) -4、B3 O3 (OH) -4、B5O6(OH) 4 -粒子。镁硼酸盐的结晶过程是一个复杂的动力学平衡过程     

Elemental abundance analyses with DAO spectrograms: XXX. The middle B through early A stars ξ2 Ceti (B9 III), 21 Aquilae (B8 II‐III), ι Aquilae (B5 III), and ι Delphini (A2V)

This series of high quality elemental abundance analyses of mostly main‐sequence band normal and peculiar B, A, and F stars defines their properties and provides data for the comparison with the analyses of somewhat similar stars and with theoretical predictions. Most use high dispersion and high S/N (≥ 200) spectrograms obtained with CCD detectors at the long camera of the Coudé spectrograph of the 1.22‐m Dominion Astrophysical Observatory telescope. Here we reanalyze 21 Aql with better quality spectra and increase the number of stars consistently analyzed in the spectral range B5 to A2 by analyzing three new stars for this series. In the early A stars the normal and non‐mCP stars have abundances with overlapping ranges. But more stars are needed especially in the B5 to B9 range. ξ² Cet on average has a solar composition with a few abundances outside the solar range while both 21 Aql and ι Aql have abundances marginally less than solar. The abundances of ι Del are greater than solar with a few elements such as Ca being less than solar. It is an Am star (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Performance of the stereoscopic system of the HEGRA imaging air erenkov telescopes: Monte Carlo simulations and observations

Based on the Monte Carlo simulations we have studied the performance of the HEGRA system of imaging air erenkov telescopes (IACTs) in its present configuration of 4 IACTs as well as in its future final configuration of 5 IACTs. Here we present the results on the basic characteristics of the IACT system which are used in the standard data analysis procedure, i.e., the collection areas, the detection rates, the angular resolution, the energy resolution, and the γ/hadron-separation efficiency. By comparing several key Monte Carlo predictions with experimental results it is possible to check the accuracy of the simulations. The Monte Carlo results concerning hadron-nuclear showers are tested with the recorded cosmic ray events and the results concerning photon-induced showers are tested with a large data sample of γ-rays observed from BL Lac object Mkn 501 during its high flaring activity in 1997. Summarizing the simulations and current observations we give the basic recommendations of using the instrument and the major values of its sensitivity.     

NOAA AVHRR 1B数据的几何精纠正

文文在对ＮＯＡＡ－ＡＶＨＲＲ像元畸变特点分析和ＩＢ格式中的定位数据质量评价基础上，确定ＩＢ格式中的定位数据。尽管绝对精度很差，但相对精度较好，可以用来进行像元的相对定位，确定像元的大小和形状，在此基础上，提出了ＮＯＡＡ－ＡＶＨＲＲ像元畸变校正方法。校正后的图像经多项式纠正后，多时相复合和与辅助数据相复合的效果很好，误差为半个像元级。