Seismic behavior of multiple reinforcement,high-strength concrete columns:experimental and theoretical analysis

This study investigates the seismic performance of multiple reinforcement,high-strength concrete(MRHSC)columns that are characterized by multiple transverse and...     

Probability distribution of the Murty‐Loomis tsunami magnitude

Abstract

In 1980, Murty and Loomis proposed a new, objective tsunami magnitude scale based on total tsunami energy. A list of 178 tsunamigenic earthquakes during the period 1815 to 1974 was given along with estimated tsunami magnitudes. In this study, we derived the probability distribution function of tsunami magnitudes based on the assumptions that (1) the occurrences of tsunamigenic earthquakes are a Poisson process, and (2) tsunami energy is a polynomial function of tsunami recurrence time. Using the data given by Murty and Loomis, the parameters of the distribution function are estimated. Comparison with the data shows that the derived distribution is a good representation of the distribution of the Murty‐Loomis tsunami magnitude.     

201002号台风“康森”移动路径特点的分析

通过对台风"康森"路径特点和影响因素的分析,特别是影响台风移动的诸多因子及其对"康森"西行北折路径所起的作用分析,发现:东亚中高纬度贝加尔湖一带为有阻塞高压的长波脊,副热带高压呈带状形势,强度强,稳定,西伸脊点偏西是"康森"稳定西偏北行的主要原因;而大尺度环境场的调整如加尔湖阻塞高压减弱、崩溃,高空槽东移加深,副高减弱东退南落,是"康森"西行北折的主要原因。同时台风中心及附近850hPa涡度场、700hPa风场的分布,对流云的发生发展也影响"康森"的移动路径。     

盾构机激光导向系统原理

以德国VMT公司的单圆盾构机为例,介绍盾构机和激光导向系统的组成,探讨激光导向系统的工作原理.重点揭示激光导向系统的测绘学原理.总结提高激光导向系统测量精度应采取的措施.     

A model of magnetically induced disc–corona for black hole binaries

We propose a model of magnetic connection (MC) of a black hole with its surrounding accretion disc based on large-scale magnetic field. The MC gives rise to transport of energy and angular momentum between the black hole and the disc, and the closed field lines pipe the hot matter evaporated from the disc, and shape it in the corona above the disc to form a magnetically induced disc–corona system, in which the corona has the same configuration as the large-scale magnetic field. We numerically solve the dynamic equations in the context of the Kerr metric, in which the large-scale magnetic field is determined by dynamo process and equipartition between magnetic pressure and gas pressure. Thus we can obtain a global solution rather than assuming the distribution of large-scale magnetic field beforehand. The main MC effects lie in three aspects. (1) The rotational energy of a fast-spinning black hole can be extracted, enhancing the dissipation in the accretion disc, (2) the closed field lines provide a natural channel for corona matter escaping from disc and finally falling into black hole and (3) the scope of the corona can be bounded by the conservation of magnetic flux. We simulate the high-energy spectra of this system by using Monte Carlo method, and find that the relative hardness of the spectra decreases as accretion rate or black hole spin a _* increases. We fit the typical X-ray spectra of three black hole binaries  (GRO J1655−40, XTE 1118+480 and GX 339−4)  in the low/hard or very high state.     

滇西试验场重力异常特征与强震潜在源区研究

本文用细化了的重力和地形综合数学模型、双层锯齿形计算模板、给定区域方差—协方差函数的最小二乘配置小区域内插和精度限定等精算重力异常场值的方法,以不低于±2.4×10~(-5)ms~(-2)和±2.9×10~(-5)ms~(-2)的精度,分别获得了滇西试验场区(99°E～102°E,24°N～27°N)最新完全布格重力异常和均衡重力异常展布图。依该区地震分布与重力场变异特征的对比研究,将下关—洱源—剑川一线划为7～7.5级地震潜在源区,永胜—大姚北划为6.5—7级地震潜在源区。     

A Clarification on the invariable point in the power-law energy spectra of non-thermal electrons of solar flares

The invariable point of non-thermal electrons was proposed two years ago, based on analyzing the two intense gamma-ray line flares observed with the X2 detector on GRS/SMM. Due to too strong hard X-ray flux in those two flares, the influence of pile-up effect might not be fully excluded. In this paper, we check the invariable point by using some medium hard X-ray events observed with HXRBS/SMM and BATSE/CGRO. It is found that the invariable point could indeed appear in some weaker hard X-ray events, in which the pile-up effect cannot play a role. Further refinement should be based on the observations with a high energy resolution. This revised version was published online in July 2006 with corrections to the Cover Date.     

耀斑谱线轮廓不对称性研究

耀斑谱线轮廓的不对称性是耀斑动力学过程的一个重要观测事实。本文在一定的耀斑半经验大气模型基础上,计算了不同速度模式和色球凝聚下的Ha和CaⅡK谱线轮廓,从半经验角度探讨了大气各个层次的速度对Hα和CaⅡK谱线轮廓的影响。结果表明:耀斑早期短时间的Hα蓝不对称性可由位于过渡区的色球凝聚引起;随后的红不对称性是上部色球物质向下运动的结果;而后来出现的CaⅡK不对称性特征则可由色球中、下部具有10—20km/s的向下速度来解释。