基于ARM7的嵌入式三维电阻率采集子站的设计研究

提出了一种基于ARM7的嵌入式三维电阻率采集子站设计方法,采用24位A/D转换器（ADS1258）和ARM7微处理器（LPC2378）,使三维电阻率法数据采集系统具有体积小、功耗低、成本低、精度高等特点,同时实现μC/OSⅡ操作系统在ARM的移植,为数据采集的实时性提供可能。     

勘察设计企业并购模式的选择

随着我国社会主义市场经济体制改革的不断深化,加入WTO后与国际市场融入度的不断加强,企业生存与发展的环境日益呈现出市场一体化、需求多元化、竞争激烈化的特征,为了拓展企业的业务范围、扩大企业规模以及提高市场的竞争实力以应对日益激烈的市场竞争,勘察设计企业面对严峻的市场和竞争环境,结合企业自身的资源、环境和并购目的选择合适的并购模式,通过借助并购等资本运营手段,将企业做大做强,增强其综合实力,有效参与全球竞争。     

基于SaaS的区域非职业体育赛事云服务平台的设计与实现

与传统软件架构模式相比,云计算具有综合成本较低、部署快速、规模调整灵活等优势,针对区域非职业体育赛事在信息采集、组织管理、赛果处理与发布等赛事运营、组织、管理等方面存在的不足,从平台构建的可行性、架构与功能等方面,讨论并实现了一种基于SaaS模式的非职业体育赛事云服务平台,最后从使用效益等方面总结该平台对于提升区域非职业体育赛事组织与管理所取得的促进作用。     

基于两种数据传输途径的国家级地面自动站逐小时数据差异分析

对2006-2009年两种途径（A文件和Z文件）上传的2400多国家级自动站观测的小时常规六要素资料进行了对比分析。结果表明：两种途径得到的小时数据中,2 min风和10 min风的不一致率较高,主要由两种文件对于风速为零时风向的规定不同造成,其他要素的不一致率相对较低;在不一致数据中,各要素在仪器误差允许范围内的比率分别为气温23.27 %、气压5.4 %、相对湿度23.19 %、降水65.42 %、2 min风12.93 %、10 min风14.16 %。     

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油企业抗震防灾规划信息管理系统的设计

基于石油企业抗震防灾工作对网络与数据库的信息管理系统的需求，对数据库产品进行了简要分析，并根据石油企业抗震防灾规划的需求和信息管理的一般模式，提出了石油企业抗震防灾规划信息计算机管理系统的设想。认为，以 Ｍｉｃｒｏｓｏｆｔ Ａｃｃｅｓｓ 数据库软件为基础，利用 Ｖ Ｂ或 Ｖ Ｃ等可视化前端应用开发工具，是目前比较好的方案，它将使石油企业抗震防灾规划工作在办公自动化方面迈向新的台阶     

Observations of pulsating Ap stars in South Africa

The rapidly oscillating Ap (roAp) stars currently represent the only main sequence stars other than the Sun which exhibit non-radial acoustic pulsations of high overtone. This makes them excellent subjects for asteroseismology, an approach which promises to yield accurate knowledge of the interior structures of stars. Of the 27 known roAp stars, 24 were discovered in Sutherland despite extensive searches conducted elsewhere. This paper reviews the discovery of the roAp phenomenon and describes the factors that contribute to the high discovery rate for these stars at Sutherland. Two long-term observational projects in progress at Sutherland are discussed,viz. the Cape roAp Star Survey and long-term monitoring of frequency variations in roAp stars.     

Photopolarimetry of 3C 66A in 2003

The BL Lac-type object 3C 66A was observed at the Crimean Astrophysical Observatory during the international project OJ-94. Observations were made over 10 nights from February through December 2003 at the Cassegrain focus of the 125-cm AZT-11 telescope with a photopolarimeter capable of simultaneous measurements in the UBVRI bands. In the course of our measurements the brightness of the object increased by more than 1 magnitude in all these bands. Its color indices varied and the degree of polarization decreased from ∼16% in February to ∼3% at the end of our observations. In December 2003 a rapid change in the position angle from 15° to 40° was noticed. The spectral energy distribution F_n is well described by a power law with a spectral index a (F_ν ∝ ν ^−α . The increase in brightness was accompanied by a reduction in the spectral index. The most probable mechanism for the observed changes in the brightness, degree of polarization, and spectral index may be a decrease in the magnetic field strength or a change in its configuration owing to a increase in the chaotic component of the field. __________ Translated from Astrofizika, Vol. 49, No. 1, pp. 41–59 (February 2006).     

Merger Dynamics of the Pair of Galaxy Clusters——A399 and A401

Convincing evidence for a past interaction between the two rich clusters A399 and A401 was recently found in the X-ray imaging observations. We examine the structure and dynamics of this pair of galaxy clusters. A mixture-modeling algorithm was applied to obtain a robust partition into two clusters, which allowed us to discuss the virial mass and velocity distribution of each cluster. Assuming that these two clusters follow a linear orbit and they have once experienced a close encounter, we model the binary cluster as a two-body system. As a result, four gravitationally bound solutions are obtained. The recent X-ray observations seem to favor a scenario in which the two clusters with a true separation of 5.4h-1 Mpc are currently expanding at 583 km s-1 along a direction with a projection angle of 67.5°, and they will reach a maximum extent of 5.65 h-1 Mpc in about 1.0 h-1 Gyr.     

SN 1998A: explosion of a blue supergiant

We present spectroscopic and photometric observations of the peculiar Type II supernova (SN) 1998A. The light curves and spectra closely resemble those of SN 1987A, suggesting that the SN 1998A progenitor exploded when it was a compact blue supergiant. However, the comparison with SN 1987A also highlights some important differences: SN 1998A is more luminous and the spectra show bluer continua and larger expansion velocities at all epochs. These observational properties indicate that the explosion of SN 1998A is more energetic than SN 1987A and more typical of Type II supernovae. Comparing the observational data with simulations, we deduce that the progenitor of SN 1998A was a massive star  (∼25 M_⊙)  with a small pre-supernova radius  (≲6 × 10¹² cm)  . The Ba  ii lines, unusually strong in SN 1987A and some faint II-P events, are almost normal in the case of SN 1998A, indicating that the temperature plays a key role in determining their strength.