面向地震烈度仪的现地地震动预测模型的构建与验证

利用初期P波预警参数构建现地地震动预测模型,使其在达到设定阈值时快速发出报警信息,是现地地震预警系统面临的一个关键问题,直接关系到发布信息的准确性和及时性。针对地震烈度仪基于微机电系统传感器记录到的数据质量较差,通过两次积分获取的位移存在较大偏差,会引起更多的误报和漏报,本文采用不同阶数（1—4阶）的巴特沃斯滤波器,分别构建了基于P波3 s和全P波段数据的位移幅值PD、速度幅值PV和加速度幅值PA与地震动峰值速度PGV和峰值加速度PGA的现地地震动预测模型,然后利用收集到的川滇示范预警网地震事件记录进行验证。结果表明,对于地震烈度仪微机电系统传感器的记录,采用1阶巴特沃斯滤波器处理、基于全P波段波形拟合获取到的PV与PGV的相关性和PA与PGA的相关性为两种最优现地地震动预测模型。具体应用时,应同时利用两种或两种以上的统计关系进行现地地震动预测,并将实际地震动观测值作为额外的判定条件,以降低误报率和漏报率。      

盐度对拟穴青蟹幼蟹存活、生长和Na+/K+-ATP 酶活性的影响

研究了盐度(6、13、20、27和33)对拟穴青蟹(Scylla paramamosain)幼蟹生长发育和Na+/K+-ATP酶活性的影响。结果表明,盐度对拟穴青蟹幼蟹甲宽和体质量特定生长率、C3蜕壳间期、甲宽增量(C1至C2和C2至C3)及Na+/K+-ATP酶活性有显著影响(P<0.05),但对幼蟹存活率、C2蜕壳间期及C3至C4甲宽增量无显著影响(P>0.05)。盐度13处理组特定生长率最高、蜕壳间期最短,盐度6处理组特定生长率最低,但与盐度20、27和33处理组无显著差异(P>0.05),而盐度33处理组蜕壳间期最长;第一次蜕壳后盐度20处理组甲宽增量最大,后两次蜕壳盐度13处理组均是最大;盐度处理0.5、4、7和11 d时,Na+/K+-ATP酶活性分别表现为盐度6>13>20>27>33、6>13>27>20>33、6>13>20>27>33和6>13>33>20>27的趋势,低盐环境下Na+/K+-ATP酶活性的升高有助于拟穴青蟹幼蟹对低渗环境的适应。     

2007年春末夏初珠穆朗玛峰地区辐射特征分析

利用2007年5月23日～6月22日的观测数据和先前已有的相关实测资料,分析了总辐射、大气逆辐射、地面长波辐射、有效辐射以及地表反射率.结果表明:春末夏初珠峰大本营地区出现瞬时总辐射大于太阳常数的现象相当频繁,甚至还能出现小时平均值也大于太阳常数的记录;由于珠峰地区海拔高,大气稀薄,低温低湿,大气逆辐射明显减少;地面长波辐射不仅低于平原地区,也低于青藏高原其他地区;在地表辐射平衡中.珠峰大本营地表有效辐射大于反射辐射;随着海拔高度的增加,白天净辐射正值持续的时间相应缩短而最大值减少.     

江门地区初春大雾的预报预警业务系统

介绍江门地区大雾天气分型预报业务系统。该系统采用Delphi语言编写程序、应用Access作为数据库进行开发,并采用人机交互方式,简化了预报流程,减少工作量,为及时、准确发布大雾预报和预警信息提供依据。该系统通过自动读取Micaps实时数据,以人工判断锋面、倒槽、切变线等有利于春季大雾的天气形势为辅助,对江门地区初春大雾天气做出客观预报,并对预报结果进行自动检验。     

阿尔泰南缘冲乎尔盆地酸性火山岩地球化学及年代学研究

阿尔泰南缘冲乎尔盆地发育一套浅变质长英质岩系,火山岩原岩为酸性凝灰质-流纹质岩。盆地岩石化学分析显示,该套火山岩为钙碱性系列,微量元素显示出与大洋板块俯冲有关的陆缘岛弧构造环境。晶屑凝灰岩的SHRIMP锆石U-Pb年代学研究表明,该套岩石的喷发年龄为436±4Ma,与盆地北缘花岗质岩石侵入时代相近(413±4Ma),属早古生代志留纪喷发而成,说明冲乎尔盆地是一个早古生代火山沉积盆地。盆地火山岩地球化学和年代学揭示,志留纪区域构造性质已经从被动大陆边缘转变为活动大陆边缘,古亚洲洋在志留纪(甚至奥陶纪)逐渐俯冲、消减,形成早古生代弧盆体系和晚奥陶世-志留纪磨拉石建造,即加里东增生陆壳(陈毓川等,2003),这种俯冲可能一直持续到泥盆纪,甚至石炭纪。从冲乎尔盆地酸性火山岩岩石学、构造环境和火山活动时代可以推断其成矿效应,盆地内产出的矿床(点)可能属于加里东期与变质-岩浆热液作用有关的有色、稀有金属-白云母成矿系列。     

The 21-cm signature of early relic H ii regions

We calculate the spin temperature and 21-cm brightness of early H  ii regions around the first stars. We use outputs from cosmological radiation-hydrodynamics simulations of the formation and evolution of early H  ii regions. In the pre-re-ionization era, H  ii regions around massive primordial stars have diameters of a few kpc. The gas within the H  ii regions is almost fully ionized, but begins recombining after the central stars die off. The relic H  ii regions are then seen as bright emission sources in hydrogen 21 cm. We make brightness temperature maps of the H  ii regions, accounting for radiative coupling with Lyman α photons in a simplified manner. The spin temperature in the relic H  ii region is close to the gas kinetic temperature, generally several hundred to several thousand degrees. We show that the relic H  ii region can be as bright as  δ T _b∼ 100 mK  in differential temperature against the cosmic microwave background for an angular resolution of subarcseconds. While individual early H  ii patches will not be identified by currently planned radio telescopes, the collective fluctuations from early H  ii regions might imprint signatures in the 21-cm background.     

An improved method for 21-cm foreground removal

21-cm tomography is expected to be difficult in part because of serious foreground contamination. Previous studies have found that line-of-sight approaches are capable of cleaning foregrounds to an acceptable level on large spatial scales, but not on small spatial scales. In this paper, we introduce a Fourier space formalism for describing the line-of-sight methods, and use it to introduce an improved new method for 21-cm foreground cleaning. Heuristically, this method involves fitting foregrounds in Fourier space using weighted polynomial fits, with each pixel weighted according to its information content. We show that the new method reproduces the old one on large angular scales, and gives marked improvements on small scales at essentially no extra computational cost.     

Constraints on primordial non-Gaussianity from a needlet analysis of the WMAP-5 data

We look for a non-Gaussian signal in the Wilkinson Microwave Anisotropy Probe ( WMAP ) 5-year temperature anisotropy maps by performing a needlet-based data analysis. We use the foreground-reduced maps obtained by the WMAP team through the optimal combination of the W, V and Q channels, and perform realistic non-Gaussian simulations in order to constrain the non-linear coupling parameter f _NL. We apply a third-order estimator of the needlet coefficients skewness and compute the  χ²  statistics of its distribution. We obtain  −80 < f _NL < 120  at 95 per cent confidence level, which is consistent with a Gaussian distribution and comparable to previous constraints on the non-linear coupling. We then develop an estimator of f _NL based on the same simulations and we find consistent constraints on primordial non-Gaussianity. We finally compute the three-point correlation function in needlet space: the constraints on f _NL improve to  −50 < f _NL < 110  at 95 per cent confidence level.     

A revisit to agglomerates of early‐type Hipparcos stars

We study the spatial structure and sub‐structure of regions rich in Hipparcos stars with blue B_T – V_T colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on‐going star formation in the Galaxy. The DBSCAN (Density‐Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early‐type stars. Once an overdensity, “agglomerate”, is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early‐type star is studied based on its heliocentric distance, proper motion, and previous spectro‐photometric information. We identify 35 agglomerates of early‐type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools. It is actually a new, nearby, young open cluster (d ∼ 470 pc, age ∼ 20 Ma) with a clear radial density gradient.We list P Puppis and other six agglomerates (including NGC 2451 A, vdBH 23, and Trumpler 10) as new sites for substellar searches because of their youth, closeness, and spatial density. We investigate in detail the sub‐structure in the Orion, CMa‐Pup and Pup‐Vel OB complexes (“super‐agglomerates”). We confirm or discover some stellar overdensities in the Orion complex, like the 25 Ori group, the Horsehead region (including the σ Orionis cluster), and the η Orionis agglomerate. Finally, we derive accurate parallactic distances to the Pleiades, NGC 2451 A, and IC 2391, describe several field early‐type stars at d < 200 pc, and discuss the incompleteness of our search. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)