The brightness of the galactic radio loops at 1420 MHz: Some indications for the existence of Loops V and VI

In this article we use 1420 MHz data to demonstrate the likely reality of Galactic radio Loops V and VI. We further estimate distances and spectral indices for both these and the four main radio loops. In the cases of Loops I–IV, radio spectral indices are calculated from the mean brightnesses at 1420 and 820/404 MHz. The spectral indices of Loops V and VI are obtained from T –T plots between 1420 and 408 MHz. Using the supernova remnant (SNR) hypothesis for the origin of radio loops, distances are calculated from the surface brightnesses and the angular diameters at 1420 MHz. We also study how results for brightnesses and distances of radio loops agree with current theories of SNR evolution. For this purpose, the ambient density and initial explosion energy of the loops are discussed. We also discuss applications of different Σ–D relations. The results obtained confirm a non‐thermal origin and nearby locations for the Galactic radio loops. Therefore, we have indications that they are very old SNRs that evolve in low ambient densities, with high initial explosion energies. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Suzaku observations of clusters of galaxies

We review results of Suzaku observations of the intracluster medium of clusters of galaxies whose O, Mg, Si, S and Fe abundances have been measured with good accuracy due to the good energy resolution and low background. Metal massto‐light ratios were derived and we will discuss the origin of the metals. We also review the results of the search for bulk motion and hard X‐ray emission. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

X‐rays from young stars: A summary of highlights from the XMM‐Newton Extended Survey of the Taurus Molecular Cloud (XEST)

The XMM‐Newton Extended Survey of the Taurus Molecular Cloud (XEST) is a survey of the nearest large star‐forming region, the Taurus Molecular Cloud (TMC), making use of all instruments on board the XMM‐Newton X‐ray observatory. The survey, presently still growing, has provided unprecedented spectroscopic results from nearly every observed T Tauri star, and from ≈50% of the studied brown dwarfs and protostars. The survey includes the first coherent statistical sample of high‐resolution spectra of T Tauri stars, and is accompanied by an U ‐band/ultraviolet imaging photometric survey of the TMC. XEST led to the discovery of new, systematic X‐ray features not possible before with smaller samples, in particular the X‐ray soft excess in classical T Tauri stars and the Two‐Absorber X‐ray (TAX) spectra of jet‐driving T Tauri stars. This paper summarizes highlights from XEST and reviews the key role of this large project. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Historical behaviour of Dome C and Talos Dome (East Antarctica) as investigated by snow accumulation and ice velocity measurements

Ice divide–dome behaviour is used for ice sheet mass balance studies and interpretation of ice core records. In order to characterize the historical behaviour (last 400 yr) of Dome C and Talos Dome (East Antarctica), ice velocities have been measured since 1996 using a GPS system, and the palaeo-spatial variability of snow accumulation has been surveyed using snow radar and firn cores. The snow accumulation distribution of both domes indicates distributions of accumulation that are non-symmetrical in relation to dome morphology. Changes in spatial distributions have been observed over the last few centuries, with a decrease in snow accumulation gradient along the wind direction at Talos Dome and a counter-clockwise rotation of accumulation distribution in the northern part of Dome C. Observations at Dome C reveal a significant increase in accumulation since the 1950s, which could correlate to altered snow accumulation patterns due to changes in snowfall trajectory. Snow accumulation mechanisms are different at the two domes: a wind-driven snow accumulation process operates at Talos Dome, whereas snowfall trajectory direction is the main factor at Dome C. Repeated GPS measurements made at Talos Dome have highlighted changes in ice velocity, with a deceleration in the NE portion, acceleration in the SW portion and migration of dome summit, which are apparently correlated with changes in accumulation distribution. The observed behaviour in accumulation and velocity indicates that even the most remote areas of East Antarctica have changed from a decadal to secular scale.     

ETM+全色波段及其多光谱波段图像的融合应用

Landsat-7ETM+的全色波段与多光谱波段有相同的太阳高度角和其他环境条件,影像获取时间一致,两种不同分辨率的数据可以不经配准而实现高精度融合。目前常用的图像融合方法很多,究竟哪种方法更适合于ETM+图像,本次试验采用HIS变换、Brovey变换、SFIM变换、加权融合4种方法,分别实现ETM+Pan与ETM+的多光谱波段的融合,并从空间纹理信息、光谱真实性2个方面进行定量和定性地评价。研究表明,从综合角度出发,基于SFIM变换的融合方法产生的光谱扭曲和失真较小,同时很大程度地保持了高分辨率的全色波段的空间纹理细节信息,是一种适合于ETM+图像融合的较佳方法。     

甘肃时段暴雨主要统计参数的水平分布规律研究

甘肃是一个干旱同时又是暴雨多发的省份。通过介绍与暴雨关系密切的甘肃自然地理概况,选用甘肃境内及其周边700个雨量站的观测资料,在统计计算10min、60min、6h、24h、3d这5个时段在每个时段的多年平均时段最大暴雨量和变差系数的基础上,研究了5个时段的两个主要统计参数在甘肃省境内的水平分布规律。对甘肃及其周边干旱地区的公路铁路建设、暴雨洪水集蓄利用、水土保持和防洪减灾等具有重要意义。     

淮北煤田太原组灰岩水年龄及同位素地球化学特征

为了解淮北煤田太原组灰岩水年龄、水化学特征及演化,采集了淮北煤田29个矿井地下水样品进行水常规、氢氧同位素及~(14)C测试。利用传统图示及统计方法探讨了地下水化学特征及演化,约束了地下水年龄及径流特征。结果表明:淮北煤田太原组灰岩水年龄在2900～21910 a之间变化,不同矿区之间灰岩水化学特征有明显差异。闸河矿区以较低的TDS浓度、最小的地下水年龄和最高的δD和δ~(18)O值为特征,为淮北煤田太原组灰岩水主要的补给区;临涣矿区孙疃矿、宿县矿区桃园矿具有较大的地下水年龄、较高的TDS浓度和低的δD和δ~(18)O值,为主要排泄区。TDS浓度等值线图和地下水年龄等值线图呈现一致的演化规律,淮北煤田东北部闸河矿区为主要补给区。太原组灰岩水径流特征主要受构造背景的控制,地下水补给条件及水岩相互作用程度决定了水体中TDS浓度和氢氧同位素富集特征。     

双轴压缩条件下颗粒材料中力链的演化

针对无黏性颗粒材料,开展了柔性边界双轴压缩数值试验,分析了不同围压下力链的数量、方向概率等随轴向应变的变化。研究结果表明：不断加载使得游离的高应力颗粒有所减少,荷载更多的被力链承担;统计意义上,力链最大长度为9个颗粒。轴向±30o范围内力链概率随应变的发展与偏应力一致,而与其邻接的[40o,60o]和[120o,140o]两个方向上的力链概率随应变的发展与偏应力相反;双轴试样剪切破坏时有单剪切带和双剪切带两种模式,当[40o,60o]和[120o,140o]两个角度区间的力链概率有较大差异时,剪切带出现在力链较少的角度区间;当这两个角度区间力链概率接近时,试样中将出现两个剪切带。     

基于快速行进迎风线性插值的微震定位算法研究

准确的微震定位方法是微震监测技术进行岩体稳定性分析的基础,而初至波走时计算方法是决定微震定位精度重要因素之一。引入一种由快速行进法(fast marching methods, FMM)与线性插值射线追踪法(LTI ray tracing)改进而来的线性插值算法,实现了在复杂岩体中相对准确的微震初至走时计算,并在均一速度模型和Marmousi模型中得到了验证。在此基础上,采用常微分方程数值算法中的单步高精度Runge-Kutta法,得到了震源点和传感器之间的射线路径,并在分层和带空洞的岩体模型中验证了其合理性。选取最小二乘法为目标函数,通过寻找目标函数值最小的方式来获得最优节点实现微震定位。在所建立的加入地下硐室的Marmousi岩体模型中,对于预设震源点的定位结果误差分别为1.41、1.00、2.83、1.41、1.41m,验证了所提方法在复杂岩体速度模型中能够实现较准确的微震定位,为进一步提高工程岩体的微震定位精度提供了新思路。     

Characteristics,differences and main controlling factors of source rocks in the central‐southern South China Sea Basins

The South China Sea is rich in oil and gas resources. With the increasing exploration of oil and gas resources in the northern South China Sea and the increasing demand for energy in the world, The central‐southern South China Sea have become important constituencies for oil and gas resources. The central‐southern basins of South China Sea can be divided into three types of basin groups, namely, the southern basin group (Zengmu Basin, Brunei‐Sabah Basin), the western basin group (Wan'an Basin, Zhong jiannan Basin) and the Central Basin Group (Liyue Basin, Beikang Basin, Nanweixi Basin and Palawan Basin). At present, the degree of exploration is relatively low, and the source rock has not yet formed a understanding of the system. The main source rock development time, source rock characteristics, hydrocarbon generation potential and control factors of each basin group are still unclear, which seriously restricts the exploration of oil and gas. Based on the sedimentary facies distribution and sedimentary filling evolution, combined with the geoche mical characteristics of the source rocks, the source age, organic matter type, hydrocarbon generation potential and main controlling factors of the basins in the central‐southern basins are discussed. By the detailed research on delta scale, provenance system, paleoclimate conditions, ancient vegetation development and hydroca rbon generation parent material, the main controlling factors of hydrocarbon generation potential of source rocks in each basin group are revealed.