往返平飘式探空在CMA-MESO三维变分中的同化及对模式预报的影响

往返平飘式探空通过一次探空气球施放实现“上升段-平飘段-下降段”三段观测,其下降段能实现在06时(世界时,下同)和18时自动垂直加密观测大气,具备提升区域高分辨率快速同化循环预报系统在06时和18时的预报技巧潜力。为了实现往返平飘式探空在区域高分辨率模式中的同化,分析其对预报的影响,初步提出了“选取模式层最接近观测”的垂直稀疏化方法来预处理资料,深入分析了稀疏化对同化效果的影响,论证了资料垂直稀疏化对于同化应用的必要性;在此基础上,开展了为期1个月的批量同化影响试验,着重分析了往返平飘式探空在长江中下游区域的组网观测对CMA-MESO模式预报技巧的影响。稀疏化敏感性试验结果表明,同化不稀疏化的往返平飘式探空相比同化传统业务探空,分析和预报误差显著增加,降水预报评分也显著降低,相反,“选取最接近模式层”数据的垂直稀疏化方案能提高模式的分析和预报技巧,表明往返平飘式探空同化前必须进行垂直稀疏化。批量同化试验结果表明,在冷启动时刻(00时和12时,为常规探空释放时刻),同化往返平飘式探空(上升段)相对同化传统业务探空,分析误差和预报误差变化较小。但在暖启动时刻(03、06、09、15、18、...     

Nonlinear numerical assessment of the seismic response of hillside RC buildings

Major damage has been reported in hilly areas after major earthquakes,primarily because of two special conditions:the variation in the seismic ground motion due to the inclined ground surface and the irregularities caused by a stepped base level in the structure.The aim of this study is to evaluate possible differences in the responses of Chilean hillside buildings through numerical linear-elastic and nonlinear analyses.In the first step,a set of response-spectrum analyses were performed on four simplified 2D structures with mean base inclination angles of 0°,15°,30°,and 45°.The structures were designed to comply with Chilean seismic codes and standards,and the primary response parameters were compared.To assess the seismic performance of the buildings,nonlinear static(pushover)and dynamic(time-history)analyses were performed with SeismoStruct software.Pushover analyses were used to compare the nonlinear response at the maximum roof displacement and the damage patterns.Time-history analyses were performed to assess the nonlinear dynamic response of the structures subjected to seismic ground motions modified by topographic effects.To consider the topographic modification,acceleration records were obtained from numerical models of soil,which were calculated using the rock acceleration record of the Mw 8.01985 Chilean earthquake.Minor differences in the structure responses(roof displacements and maximum element forces and moments)were caused by the topographic effects in the seismic input motion,with the highly predominant ones being the differences caused by the step-back configuration at the base of the structures.High concentrations of shear forces in short walls were observed,corresponding to the walls located in the upper zone of the foundation system.The response of the structures with higher angles was observed to be more prone to fragile failures due to the accumulation of shear forces.Even though hillside buildings gain stiffness in the lower stories,resulting in lower design roof displacement,maximum roof displacements for nonlinear time-history analyses remained very close for all the models that were primarily affected by the drifts of the lower stories.Additionally,vertical parasitic accelerations were considered for half the time-history analyses performed here.The vertical component seems to considerably modify the axial load levels in the shear walls on all stories.     

RCP4.5情景下预测21世纪南海海平面变化

结合卫星高度计资料和SODA温盐数据,本文利用CCSM(Community Climate System Model version4)气候系统模式在代表性浓度路径RCP4.5情景下对全球海平面变化趋势的预测模拟结果作为强迫场,用POP模式模拟预测21世纪南海海平面长期趋势变化及空间分布。模拟结果显示,在RCP4.5情景下,南海海域在21世纪末10年平均海平面相对于20世纪末10年上升了15~39cm,明显上升海域位于中南半岛东部的南海中部、南部海域和吕宋海峡东西两侧海域,上升值最大可达39cm。如果加上格陵兰和南极等陆地冰川融化的影响,21世纪南海总海平面上升值将可能达到35~75cm。南海比容海平面明显上升区域位于吕宋岛东面的深水海域,广东沿岸流和吕宋冷涡之间海域,以及中南半岛东南部海域。总比容海平面的变化主要来自热比容,盐比容贡献比较小。南海南部和西部比容海平面上升速率较低,如加里曼丹岛西北侧、泰国湾和海南岛西侧有下降趋势。     

两种海浪模式对中国黄海海域浪高模拟能力的比较

本文利用第三代海浪数值模式WAVEWATCH和SWAN模式,分别对黄海区域进行了理想模拟计算和实际浪场的模拟计算,结果表明:理想状态下两种模式的模拟结果在大小和空间分布上都不相同,但在大小及其变化趋势士相差不大;在实际模拟中,将两种模式的模拟结果与实际观测值相比,发现SWAN模式模拟结果较WAVEWATCH模式好,只是在高风速的模拟情况下,SWAN模式模拟结果偏大,而WAVEWATCH模式模拟结果偏小.     

海洋石油烃降解细菌T1和T2的分子鉴定分类

从天津滨海潮间带被石油烃严重污染的沉积物（千样含油量0．2g／g）中,筛选分离出能够以柴油为唯一碳源生长的细菌,对其中生物量大、单株菌降解效率较高的两株细菌T1和T2进行16SrDNA克隆,通过测定和比较16SrDNA的部分序列对这两株细菌进行分子鉴定,以期用于石油污染的微生物修复中。结果表明,T1与深红红螺菌（Rhodospirillum rubrum）的同源性为89％,．r2与施氏甲单孢杆菌（Pseudomonas stutzeri）的同源性为99％。     

Broadband submillimeter measurements of the full Moon center brightness temperature and application to a lunar eclipse

We report on observations of the full Moon brightness temperature covering the frequency range of 300-950 GHz, and also on observations of the lunar eclipse of July 16, 2000, though only covering the frequency range of 165-365 GHz due to poor atmospheric transmission at higher frequencies. All observations were performed from the summit of Mauna Kea (HI) using a Fourier Transform Spectrometer mounted on the Caltech Submillimeter Observatory and supplemented by measurements of the atmospheric opacity using a 183 GHz Water Vapor Monitor. The telescope was pointed to the center of the lunar disk (with a footprint of ∼45-15 km on the Moon at 300 through 900 GHz). In order to obtain the correct values of the Moon brightness temperatures at all frequencies we carefully corrected for the atmospheric absorption, which varies across the submillimeter domain. This correction is fully described. The measured pre-eclipse brightness temperature is around 337 K in the 165-365 GHz range. This temperature slightly increases with frequency to reach ∼353 K at 950 GHz, according to previous broader band data. The magnitude of the temperature drop observed during the eclipse at 265 GHz (central frequency of the band covered) was about ∼70 K, in very good agreement with previous millimeter-wave measurements of other lunar eclipses. We detected, in addition, a clear frequency trend in the temperature drop that has been compared to a thermal and microwave emission model of the lunar regolith, with the result of a good match of the relative flux drop at different frequencies between model and measurements.     

太阳磁场理论外推研究进展

太阳磁场是研究太阳物理的关键。目前对太阳磁场的精确测量只限于光球层。对日冕磁场结构的了解,则多是以观测的光球磁场作为边界条件,在某种理论模型下进行外推。势场模型、线性无力场模型和非线性无力场模型是无力场假设下的三种理论外推模型。文章介绍了太阳磁场理论外推的基本方法和最新进展,和对三种模型中使用较多的外推方法,列举了它们在天文研究中的一些应用,同时也简略讨论了外推方法中存在的一些问题。     

柴达木盆地矿产开发中环境地质问题及防治对策

在柴达木盆地环境现状实际调查基础上，根据调查资料论述了柴达木盆地地区矿产开发引起的主要环境地质问题及其危害。分析了引起土地沙化．土壤盐渍化，水土污染，崩塌地面塌陷，生态环境恶化产生原因，并在地质环境保护方面提出合理化建议，以期为西部开发过程环境保护提供依据。     

The Neutrino Telescope Antares

Whilst the number of observed astrophysical sources of γ-rays is now moderately high, only three astrophysical objects have been studied with neutrinos, namely the Sun, a supernova (SN1987A) and the Earth (its atmosphere). However, astro-neutrinos may give a new boost to astrophysics, similar to the impressive progress provided during the last decades by γ-rays. The ANTARES collaboration aims to build a large neutrino telescope under the Mediterranean Sea at a depth of 2500 m. To reach this goal, a remarkable effort of R&D has been performed in recent years that has culminated in the deployment, connection and operation of two prototype strings. The final detector will be composed of 12 strings and will be ready by 2007.