Swift observations of CSS081007:030559+054715

CSS081007:030559+054715 was discovered by the Catalina Real‐time Transient Survey. Optical spectroscopy revealed a multi‐peaked Hα emission line profile with radial velocities exceeding 1500 km/s, as well as strong Ne emission, suggestive of a neon nova. We monitored the source extensively with the Swift satellite, obtaining a unique dataset spanning 270 days in the soft X‐ray and UV bands. The data reveal a soft, blackbody‐like spectrum with a temperature around 55 eV (though dependent on the modelling), variable X‐ray and UV light curves with a 1.77 day period in both the X‐ray and UV bands, a longer timescale modulation of ∼ 50 days, followed by a slowly declining trend in the soft X‐ray and UV flux. We highlight the Swift observations and their implications for the SSS nature of this object (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Numerical study of two‐phase fluid distributions in fractured porous media

Two‐phase fluid distributions in fractured porous media were studied using a single‐component multiphase (SCMP) lattice Boltzmann method (LBM), which was selected among three commonly used numerical approaches through a comparison against the available results of micro X‐ray computed tomography. The influence of the initial configuration and the periodic boundary conditions in the SCMP LBM for the fluid distribution analysis were investigated as well. It was revealed that regular porous media are sensitive to the initial distribution, whereas irregular porous media are insensitive. Moreover, to eliminate the influence of boundaries, the model's buffer size of an SCMP LBM simulation was suggested to be taken as approximately 12.5 times the average particle size. Then, the two‐phase fluid distribution of a porous medium was numerically studied using the SCMP LBM. Both detailed distribution patterns and macroscopic morphology parameters were reasonably well captured. Finally, the two‐phase fluid distributions in a fractured porous media were investigated. The influence of the degree of saturation, fracture length, and fracture width on the fluid distributions and migration was explored. Copyright © 2015 John Wiley & Sons, Ltd.     

利用扫描电镜和X射线衍射仪对滑坡滑带土的研究

利用扫描电子显微镜（SEM）和X射衍射仪（XRD）研究了三峡库区，黄河小浪底等地40个滑坡滑带土的结构及物质组合，指出当滑坡处于滑动阶段时，滑带土表居可见粘土矿物定向排列，普遍可见擦痕（弧型，线型，紊乱型），微裂隙和微空隙发育，微生物较多，当斜坡处于稳定阶段时，岩层软弱带可见粘土矿物无定向排列，表面无擦痕，常见树枝状结构。滑带土的物质组合主要为：蒙脱石，蛭石，伊利石，高岭石，绿泥石，方解石，石英，长石和微生物，而蒙脱石，蛭石和微生物含量是滑坡滑动的一个重要因素。据微结构的变化和物质组合可以分析滑坡的活动次数，活动阶段和形成机理，为滑坡治理和稳定性评价提供依据。     

理学ZSX系列X荧光光谱仪中文软件开发

介绍了日本理学ZSX系列X荧光光谱仪的特点和新开发的中文版软件的功能。     

江苏北部龙卷雷达组网探测策略

为了探测、分析和研究尺度小、生命史短、致灾重的龙卷等强对流天气三维精细化垂直结构及演变规律,江苏正在龙卷易发区苏北平原建设高时空分辨率的双偏振雷达网。本文为支撑苏北龙卷雷达网建设,从龙卷雷达组网的必要性出发,重点分析苏北龙卷雷达组网策略。研究表明:(1)苏北龙卷雷达网拟采用大天线、全固态、高性能技术指标的X波段双偏振雷达组网,采用不同的观测模式,可获得空间一致性好、时空分辨率高且丰富的探测数据,满足龙卷等强对流天气的快速、精细化探测要求。此外,采用较高的脉冲重复频率等扩展测速范围,解决X波段雷达速度模糊问题。(2)经理论计算与比较,苏北龙卷雷达网可采用正三角形组网拓扑结构,取累计空间密度值90%,雷达间距为60km时,波束直径b_s特征值为282.0m,最低波束高度b_h特征值为52.6m,探测灵敏度Z_(min)特征值为2.7dB;X波段雷达组网与S波段业务雷达相比,在60km探测距离处,其波束直径减小了约2倍,0°仰角盲区高度降低了约1.5倍,探测灵敏度降低了2.4dB。即在方位分辨率、探测盲区、弱回波探测能力、数据空间一致性等方面均得到提升,可提供更多低于1km、甚至百米的高时空分辨率的雷达资料,便于捕捉龙卷等强对流天气。(3)苏北龙卷雷达网在盐都、阜宁、大丰、宝应、兴化(龙卷易发区),各布设一部固定式X波段全固态双偏振多普勒天气雷达。综合考虑在苏北平原雷达选址的各种因素,最终雷达网基本单元拟采用近似正三角形(N=3,L=45～65km)的拓扑结构。5部高时空分辨率的龙卷探测雷达组成3个近似正三角形的单元,镶嵌在S波段雷达业务网内(盐城、淮安、泰州雷达中间)。后续可进一步增加雷达数量及拓宽观测区域,例如在高邮等龙卷易发地区,可增补X波段天气雷达或C波段相控阵天气雷达。     

磁层顶的涡旋诱发重联和单X线重联

用二维MHD数值模拟研究了地球磁层顶的涡旋重联和单X线重联,并将两者作了比较。涡旋重联和单X线重联各在Alfvèn马赫数M_Λ大于和小于0.5时出现于向阳面磁层顶。前者所产生的磁岛与涡旋同心重叠;后者磁力线重联仅产生X点,而不闭合形成磁岛,涡旋分布于X点两侧。在涡旋重联的自组织过程中,互螺旋度等近似守恒决定其渐近态的拓扑结构。最后,讨论了这两种重联对通量传输事件所起的不同作用。     

山西峨嵋台地的挤压型地裂

考察了山西峨嵋台地万荣城区一带的挤压型地裂,发现其呈北西-南东的条带状,1985年发生,至今仍在发展。地裂带上墙砖、水泥地砖拱曲翘起,水泥地面条带状拱曲,土体发育呈波浪条带状垅岗;墙体开裂,墙体裂缝中间宽上下两头细,地裂带上X型破裂发育。分析了万荣城区一带地裂的特征,讨论了万荣挤压型地裂的力学成因机制。     

聚类分析法在地质样品分类中的应用研究

概述聚类分析及原理,通过题示内容的研究,包括测试样品,标准化数据,分类,获得适宜的样品聚类分析方法及建立了方法软件。该研究实验表明,采用聚类分析法对地质样品进行分类,效果较好。为开展Ｘ荧光定量分析及建立模式识别专家系统奠定了基础。     

An alternative to O−C analysis of variable star periods

For more than a century now astronomers have used the O−C (Observed minus Calculated) method to detect the presence of systematic changes in the periods of variable stars. The method is based on an analysis of residuals from a linear fit to the observed epochs. A rather common error in applications of the method is a failure to make provision for autocorrelation which exists in the data. In this paper we consider a model that accounts for the presence of autocorrelation and develop an alternative to the O−C method of analysis. The proposed method focuses on the frequency domain characteristics of observed periods. Its use is illustrated by application to data from the variable stars X Aurigae and RY Sagittarii.     

硅酸盐玻璃和熔体中硅和铝的配位与局部结构:K边X射线吸收光谱研究

硅酸盐玻璃和熔体中硅和铝的配位与局部结构：Ｋ边Ｘ射线吸收光谱研究＊李迪恩（中山大学地质系，广州５１０２７５）关键词硅酸盐玻璃和熔体硅和铝的配位Ｘ射线吸光谱高压下硅酸盐矿物和玻璃中的硅可以形成八面体配位［１］，但在通常的低压硅酸盐玻璃中，硅和铝为四面体...