Dynamic response analysis of a floating mooring system

An innovative floating mooring system with two or more independent floating mooring platforms in the middle and one rigid platform on each side is proposed for improving efficiency and safety in shallow water. For this new system, most of collision energy is absorbed through the displacement of floating platforms. In order to illustrate the validity of the system, a series of model tests were conducted at a scale of 1:40. The coupled motion characteristics of the floating mooring platforms were discussed under regular and irregular waves, and the influences of wave direction and other characteristics on dynamic response of the system were analyzed. The results show that the mooring system is safest at 0° of wave incident angle, whereas the most dangerous mooring state occurs at 90° of wave incident angle. Motion responses increase with the increase of wave height, but are not linearly related to changes in wave height.     

聚焦“协调”,增进对人地协调观的理解

人地协调观因突出强调“协调”而不等同于人地观(念)。溯源人地关系原理,“协调”主要体现在人与地之间物质、能量的流通量和流通程度都需要控制在合理的“极限值”以内,依靠科学的行动与调适,确保人地交互状况运行在合理区间当中。本文聚焦“协调”,将以往用“地对人的影响”“人对地的影响”和“人地和谐发展”来解构人地协调观素养表现的方法,进一步调适、概括为:“辩证看待地理环境对人类的影响”“懂得人类活动需尊重自然规律”“综合评判人地关系问题和举措”,通过协调认识、协调应对和协调评价三个方面充分突出“协调”意蕴。     

虹鳟(Oncorhynchus mykiss)、溪红点鲑(Salvelinus fontinalus)及杂交种(虹鳟×溪红点鲑) 血清蛋白多态性的研究

提要 利用非变性聚丙烯酰胺凝胶电泳法,对虹鳟、溪红点鲑及杂交种(虹鳟♀溪红点鲑♂)的进行了血液蛋白多态性研究, 计算了各座位的基因频率、基因纯合度和Shannon 信息指数, 并探讨了群体间的亲缘关系和遗传距离。结果表明: ( 1) 3个种群在α球蛋白、β1球蛋白、γ-球蛋白、前白蛋白和白蛋白5个座位上的遗传差异较大, 血清蛋白座位的优势基因在不同群体中有不同的频率; ( 2) 杂交种中出现部分双亲特异条带,表明杂交种整合了虹鳟♀ 和溪红点鲑♂的遗传信息,属两性融合生殖, 是真正意义上的杂交种。( 3) 杂交种与虹鳟和溪红点鲑的遗传相似性系数分别为0.718和0.575, 遗传距离分别为0.332和0.554, 表明杂交种与两亲本的遗传差异不是对等的, 而是偏向母本一方, U PGMA 系统树也同样证明了这一点。     

网络RTK在活动构造变形分析中的应用——以川西南大塘断裂为例

在活动构造研究方面,传统RTK技术常用于局部的地表测量,测量距离受限于信号的地形影响。而网络RTK技术基于全国区域性的基准站网,通过移动通信可以实现百公里以上尺度厘米级精度动态测量,在构造地表分析方面具有广阔应用空间。本文以横跨龙门山地区的大塘断裂为试验对象,利用网络RTK技术测量了一条长度17.7 km的地表剖面。测量结果表明,尽管大塘断裂局部受到强烈的侵蚀作用不易识别,但网络RTK测线能够反映出区域性的褶皱变形特征。结合深部地震剖面进行定量分析发现,地表的冲积扇发生反坡向的构造抬升,与深部的断层扩展褶皱变形对应。进一步参考年代学数据计算得出,横跨大塘断裂的第四纪构造缩短速率为0.29±0.04 mm/yr。试验分析结果表明,网络RTK技术可以用于大尺度、高精度的构造变形分析,识别区域性的构造变形。

     

A hybrid analysis method for linear dynamic soil-structure interaction in time and frequency domain

IntroductionThe analysis of dynamic soil-structure interaction for important engineering project is still based on linear model (including equivalent linear model) with complex damping, and traditional frequency domain method (Lysmer, et al, 1975, 1981; DING, et al, 1999). Namely, first calculating frequency domain solution by Fourier transform, and then calculating time domain solution by Fourier inverse transform. The motion equation of a system in frequency domain is usually written as (…     

Measurements of spectral lines observed with Hinode/EIS as implications for coronal heating

We have measured the line widths and nonthermal velocities in 12 solar regions using high resolution EUV data taken by Hinode/EIS. We find that there exists a positive correlation between the intensity and nonthermal velocity for the Fe XII emission line as well as some other lines. The correlation coefficients decrease from the disk center to the limb. However, the nonthermal velocities of a particular spectral line do not vary much in different regions, so they are considered isotropic. In particular, we find that for a coronal loop structure, the largest widths and nonthermal velocities occur at the footpoints, where outflows appear. Based on these observational results, we discuss several physical processes responsible for coronal heating.     

Low-velocity structure beneath Africa from forward modeling

Seismic waveforms observed in South Africa containing the first arrival crossover of S to SKS (70° to 110°) are analyzed. The data consist of analog records from the World Wide Seismographic Station Network (WWSSN) of deep events beneath South America. The S-waves arrive 2 to 3 s early relative to PREM at ranges from 70° to 95° and then become increasingly delayed, becoming 5 to 6 s late at 110°. The SKS phase is late by 3 to 5 s over the entire range. This pushes crossover between S and SKS, normally observed at about 81°, out about 2° to 3°, which is the most anomalous shift ever reported. To model such features, we modified Grand's tomography model [Grand et al., GSA Today 7 (1997) 1–7], and generated 2D synthetics to match the data. The overall shape and position of the lower mantle low-velocity anomaly proposed by Grand predicts good results if lower mantle anomalies are enhanced to a level of about 4%. This results in a complex tabular structure extending upward from the core–mantle boundary about 1500 km into the mantle. These features appear to be consistent with a large young plume which is erupting off the CMB.     

Climatic implications of loess deposits from the Beijing region

Variations in magnetostratigraphy, pedostratigraphy, grain size and magnetic susceptibility of the loess deposits near Beijing have been studied at two sections. The sections are about 400 km east of the main loess deposits in China, have a maximum thickness of 100 m and extend back to 1.1 Ma. The sequence consists of 14 loess–palaeosol couplets (S0‐S14), which correlate well with sequences in the Loess Plateau. Susceptibility records from the sites near Beijing are comparable to the Xifeng, Luochuan and Baoji sections located in the middle part of the Loess Plateau; however, the down‐core variations in the grain size in the Upper Lishi Formation exhibit some differences. The median grain size increases by about 25–30 µm from L4 to L2, with the sandy grains (>63 µm) increasing from 10–20 wt% to 40–50 wt% . This implies that the depositional environment of the dust sources in the Beijing loess section is different in some aspects from the Loess Plateau. The Beijing loess may have had a different dust source than the Loess Plateau. Copyright © 2001 John Wiley & Sons, Ltd.     

The role of non-thermal electrons in the hydrogen and calcium lines of stellar flares

There is observational evidence showing that stellar and solar flares occur with a similar circumstance, although the former are usually much more energetic. It is expected that the bombardment by high-energy electrons is one of the chief heating processes of the flaring atmosphere. In this paper we study how a precipitating electron beam can influence the line profiles of Ly α , H α , Ca  ii K and λ 8542. We use a model atmosphere of a dMe star and make non-LTE computations taking into account the non-thermal collisional rates owing to the electron beam. The results show that the four lines can be enhanced to different extents. The relative enhancement increases with increasing formation height of the lines. Varying the energy flux of the electron beam has different effects on the four lines. The wings of Ly α and H α become increasingly broad with the beam flux; change of the Ca  ii K and λ 8542 lines, however, is most significant in the line centre. Varying the electron energy (i.e. the low-energy cut-off for a power-law beam) has a great influence on the Ly α line, but little on the H α and Ca  ii lines. An electron beam of higher energy precipitates deeper, thus producing less enhancement of the Ly α line. The Ly α /H α flux ratio is thus sensitive to the electron energy.