伽师近场观测地震资料的三维Q值成像

为了研究震源区介质的物性特征,利用振幅谱拟合和有限差分三维Q值成像方法处理了伽师地震区临时台网的地震波形资料,获得了该地震区上地壳的S波三维Q值图像。结果表明:不同深度的Q值图像都存在低Q值带,主要展布方向为EW向、NNE向和NNW向,与研究区的柯坪断裂、羊达曼断裂和麦盖提断裂有一定的对应关系,并且NNE向的低Q值带与强震群分布和余震分布的条带位置接近,推测低Q值带可能是震源区的几条深部断裂。     

论环渤海地区资源结构与产业结构特点

环渤海地区是一个资源型产业聚集区,其产业结构的形成与特点同资源结构间有着密切的联系.本区资源结构特点可以概括为光、热、水、土资源组合较好,矿产资源丰富且矿种配套较佳、钢铁和化工工业生产条件理想,水资源不足、水土和水矿结构不尽理想.在资源结构基础上形成了本区产业结构中第一产业基础较好,第二产业强大、采掘和原材料工业突出,第三产业相对比较落后的特点.这些特点是环渤海地区今后产业结构升级转换的主要影响因素.     

华北地区上部地壳结构的三维有限差分层析成像

采用正方形网格对华北地区速度模型进行参数化、网格维数为649×90×16,网格间距为1km. 通过对华北地区30条深地震测深剖面的Pg波三维有限差分速度层析成像反演,获得了该地区上部地壳的三维速度结构. 反演结果显示,低速的"棱形"华北盆地被高速的隆起所包围;而华北盆地又由两个大的断陷带中间夹一个隆起所组成.两个大的断陷带又被分割为多个小的断陷盆地.研究区内的断层多为铲式正断层,结晶基底深度变化较大. 所有这些表明华北地区具有复杂的地质构造和发生强震的深部背景.     

东昆仑西大滩盆地晚新生代构造地貌简析

东昆仑山脉的南缘,发育一条巨型的以左行走滑为主的活动断裂带,其中西大滩左行走滑断裂是东昆仑断裂带的一部分,控制着西大滩盆地的构造地貌演化。本研究在野外调查了西大滩盆地内部和盆地边缘的活动断裂,测量了这些断层的几何学参数,并对其运动学进行了研究。研究认为,晚新生代以来西大滩盆地中心发育有西大滩左行走滑断裂,而在盆地南北两侧则发育有伸展变形,存在一系列活动的高角度脆性正断层,可见清晰的断层三角面构成盆地南北两侧的山坡。这些正断层呈阶梯状产出,向盆地内部倾斜,与盆地中心的左行走滑断裂一起,在剖面上构成负花状构造,证明西大滩盆地发生了张扭性变形。走滑断裂的走滑运动往往伴随构造转换现象,在断裂弯曲或侧接部位可以形成走滑拉分盆地。西大滩盆地从其盆地形态来看,是一个狭长的张扭性盆地,盆地长宽比值约为7.5~30.0之间,大于7︰ 1,不符合典型的走滑拉分盆地的特征;控制西大滩盆地的西大滩走滑断裂并未见明显的弯曲,从而排除盆地的走滑拉分成因。本文认为西大滩盆地的形成与西大滩断裂本身的张扭性变形直接相关,反映了该地区区域上处于张扭性而非压扭性应变状态,其成因与上地壳刚性变形和下地壳塑性流变密切相关;西大滩地区构造地貌的演化受控于晚新生代以来青藏高原下地壳通道流(channel flow)的活动。结合前人的研究成果认为东昆仑活动断裂带晚期的张扭性活动可能起始于至少7Ma B.P.以前或10±2Ma B.P.,且在昆仑山垭口盆地断陷形成时期(3.6Ma B.P.)活动更加强烈,在0.6Ma B.P.的"昆仑-黄河运动"时期可能达到顶峰,奠定了东昆仑西大滩地区现今的构造地貌格局。     

Crustal structure of the western Arafura Sea from ocean bottom seismograph data

Refraction data taken from ocean bottom seismograph recordings in the western Arafura Sea indicate a continental‐type structure for the region. This structure is characterised by a thin column (2 km) of sediments, with velocities ranging from about to 2 to 4 km s^‐1, overlying an essentially two layer crust. The compressional wave velocities in the upper and lower crust are 5.97 and 6.52 km s^‐1, respectively, with the boundary between the layers at a depth of 11 km. Very weak mantle‐refracted arrivals with a velocity of about 8.0 km s^‐1 were recorded. Large‐amplitude, later arrivals, beginning at distances near 100 and 150 km, have been interpreted to be part of the retrograde branches from the 8.0 and 7.33 km s^‐1 layers, respectively. Model studies indicate that a small positive velocity gradient is required between 17 and 30 km, and that the Moho is at a depth of 34 km. A third set of large amplitude, later arrivals starting at a distance near 250 km has been interpreted as most probably multiple refraction‐reflection arrivals from the 5.97 and 6.52 km s^‐1 layers. Correlation of this structure with the stratigraphic logs from exploratory oil wells in the Arafura Sea using layer velocities indicates that rocks younger than Jurassic appear to thin towards the east.     

丽江—攀枝花—者海地带二维地壳结构及其构造意义

本文利用攀西地区通过攀枝花的东西向剖面爆炸地震资料,进行了震相的重新识别和二维射线追踪与理论图计算.结果表明,沿剖面地表附近有4个低速区和若干高速带,它们与地质和构造有很好的对应关系.渡口附近的高速岩体一直延伸到了上地壳的底部,形成一个统一的地垒状构造,该高速体与攀枝花成矿岩体相关,并推断华坪及其以西地带也是找矿的有利地区.中地壳下部有一厚度约9km的低速层,它可能是壳内的韧性剪切带.低速层顶部深度为27.0—29.5km,与研究地区的居里面深度及天然地震震源深度的分布基本符合.剖面东段中地壳顶部还有一层很薄的低速层,反映了构造带两侧运动的不对称性.地壳厚度为53—56km,构造带中部的Moho界面没有明显的上隆.     

Response of a Resilient Community to Natural Disasters: The Gorkha Earthquake in Nepal, 2015

The ability of a community to withstand and recover from adversities including natural and man-made disasters has emerged as a major policy issue in recent years. This research aims to assess the role of institutional initiatives in building resilient communities and their response to natural disasters like the Gorkha earthquake in Nepal in 2015. The work is based on data collected from primary and secondary sources along with field observations. It is evident that resilient communities are equipped with greater coping capacities in the face of natural disasters and have reduced vulnerability to future hazards. Institutional capacity building and resilient construction including the School Earthquake Safety Program ensured better disaster preparedness. The traditional open spaces and building designs added to the structural resilience. There is, however, a need to build back better and to communicate earthquake-resistant designs to the affected communities.     

Evolution of peaks in weakly non-linear density field and dark halo profiles

Using the two-point Edgeworth series up to second order in the linear rms density fluctuation we construct the weakly non-linear conditional probability distribution function for the density field around an overdense region. This requires calculating the two-point analogues of the skewness parameter S ₃. We test the dependence of the two-point skewness on distance from the peak for scale-free power spectra and Gaussian smoothing. The statistical features of such a conditional distribution are given as the values obtained within linear theory corrected by the terms that arise as a result of weakly non-linear evolution. The expected density around the peak is found to be always below the linear prediction while its dispersion is always larger than in the linear case. For large enough overdensities the weakly non-linear corrections can be more significant than the peak constraint introduced by Bardeen et al. We apply these results to the spherical model of collapse as developed by Hoffman & Shaham and find that in general the effect of weakly non-linear interactions is to decrease the scale from which a peak gathers mass and therefore also the mass itself. In the case of an open universe this results in steepening of the final profile of the virialized proto-object.     

Distant field blue horizontal branch stars – III. Identification of a probable outer halo stream at Galactocentric distance r= 70 kpc

We present FOcal Reducer/low dispersion Spectrograph-1 spectra (from the European Southern Observatory's Very Large Telescope) of a sample of 34 faint  20.0 < g * < 21.1  A-type stars selected from the Sloan Digital Sky Survey Early Data Release, with the goal of measuring the velocity dispersion of blue horizontal branch (BHB) stars in the remote Galactic halo,   R ∼ 80 kpc  . We show that colour selection with  1.08 < u *− g * < 1.40  and  −0.2 < g *− r * < −0.04  minimizes contamination of the sample by less luminous blue stragglers. In classifying the stars we confine our attention to the 20 stars with spectra of signal-to-noise ratio >15 Å⁻¹. Classification produces a sample of eight BHB stars at distances  65–102 kpc  from the Sun (mean 80 kpc), which represents the most distant sample of Galactic stars with measured radial velocities. The dispersion of the measured radial component of the velocity with respect to the centre of the Galaxy is  58 ± 15 km s⁻¹  . This value is anomalously low in comparison with measured values for stars at smaller distances, as well as for satellites at similar distances. Seeking an explanation for the low measured velocity dispersion, further analysis reveals that six of the eight remote BHB stars are plausibly associated with a single orbit. Three previously known outer halo carbon stars also appear to belong to this stream. The velocity dispersion of all nine stars relative to the orbit is only  15 ± 4 km s⁻¹  . Further observations along the orbit are required to trace the full extent of this structure on the sky.