三峡工程库首区及狮子口重力滑动构造系统的构造应力场研究

基于野外实测和室内测试,计算分析及有限元模拟,对三峡工程库首区燕山期和喜山期的区域构造应力场以及狮子口重力滑动构造应力场进行研究。区域构造应力场的主要特征是：燕山主期σ1和σ1近水平,分别近S－N向和E－W向,σ2近直立,差异应力200MPa、变化范围150－250MPa;喜山主期σ1近水平,总体方向NNE70－SW250°,差异应力100MPa,变化范围80－120MPa,在空间变化上,前者表现为南部差异应力高于北部差异应力,后者的变化规律不太明显。狮子口重力滑动构造系统的应力场比较复杂,总体呈近E－W向的前缘挤压、后缘拉伸,而滑动系统内部叠置产出的三个滑块也分别表现出后缘拉伸、前缘挤压并交替出现的特点,反映了区域应力场背景下的局部构造应力场特征。     

临界曲线附近的微引力透镜效应模拟

在光滑物质分布模型下,临界曲线是强引力透镜系统中像平面上一条放大率为无穷的线,而考虑少量离散质量的微透镜效应后,源平面上的放大率分布会出现复杂的结构,为暗物质成分的探测提供了一种有效途径.模拟临界曲线附近微透镜效应存在临界曲线上放大率无穷大和计算量巨大的困难.要达到所需的模拟精度,直接使用传统的光线追踪算法需要巨大的计算资源.为此发展了一个能实现海量计算的Graphics Processing Unit (GPU)并行方法来模拟临界曲线附近的微引力透镜效应.在型号为NVIDIA Tesla V100S PCIe 32 GB的GPU上,对于需要处理13000多个微透镜天体、发射1013量级光线的模拟,耗时在7000 s左右.在GPU并行的基础上,与直接的光线追踪算法相比,插值近似的引入使计算速度提升约两个数量级.利用该方法生成80个放大率分布图,并从中抽取800条光变曲线,进行了微焦散线数密度和峰值放大率的统计.     

计算Legendre函数导数的非奇异方法

引力场关于经度和纬度方向的梯度在两极附近会产生奇异性现象,这将会给诸如重力场和静态洋流探索(GOCE,Gravity field and stesdy-state Oceam Circulation Explorer)数据处理等引力场的研究工作带来诸多不便和困难。这里首先分析了该奇异性产生的原因,即目前采用的球坐标系自身在两极处是奇异的;然后利用Legendre函数的性质推导了一组不含任何奇异性的计算引力场梯度的计算公式;最后与常用的迭代方法进行了实例计算比较,结果表明所导出的公式不仅计算精度大大提高,而且计算用时也不会增加。     

Using galaxy redshift surveys to detect gravitationally lensed quasars

Gravitationally lensed quasars can be discovered as a by-product of galaxy redshift surveys. Lenses discovered spectroscopically in this way should require less observational effort per event than those found in dedicated lens surveys. Further, the lens galaxies should be relatively nearby, facilitating a number of detailed observations that are impossible for the more common high-redshift lenses. This is epitomized by the wide range of results that have been obtained from Q 2237+0305, which was discovered as part of the Center for Astrophysics redshift survey, and remains the only quasar lens discovered in this way. The likelihood of this survey yielding a lens is calculated to be ∼0.03, which is an order of magnitude larger than previous estimates due to two effects. First, the quasar images themselves increase the observed flux of the lens, so that lens galaxies up to a magnitude fainter than the nominal survey limit must be included in the calculation. Secondly, it is possible for lensed quasars with extremely faint deflectors to enter the survey due to the extended morphology of the multiple images. Extrapolating these results to future surveys, the 2 degree Field galaxy redshift survey should contain between 10 and 50 lenses and the Sloan Digital Sky Survey should yield between 50 and 300 lenses, depending on the cosmological model and the observing conditions.     

The statistics of wide-separation lensed quasars

The absence of any wide-separation gravitational lenses in the Large Bright Quasar Survey is used to place limits on the population of cluster-sized haloes in the universe, and hence constrain a number of cosmological parameters. The results agree with previous investigations in strongly ruling out the standard cold dark matter model but they are consistent with low-density universes in which the primordial fluctuation spectrum matches both cluster abundances and cosmic microwave background measurements. These conclusions are essentially independent of the cosmological constant, which is in stark contrast to the statistics of galaxy lenses. The constraints presented here are nullified if clusters have core radii of ≳10 kpc, but are free of a number of potential systematic errors, owing to the homogeneity of the data.     

Infrared observations of gravitational lensing in Abell 2219 with CIRSI

We present the first detection of a gravitational depletion signal at near-infrared wavelengths, based on deep panoramic images of the cluster Abell 2219 ( z =0.22) taken with the Cambridge Infrared Survey Instrument (CIRSI) at the prime focus of the 4.2-m William Herschel Telescope. Infrared studies of gravitational depletion offer a number of advantages over similar techniques applied at optical wavelengths, and can provide reliable total masses for intermediate-redshift clusters. Using the maximum-likelihood technique developed by Schneider, King & Erben, we detect the gravitational depletion at the 3 confidence level. By modelling the mass distribution as a singular isothermal sphere and ignoring the uncertainty in the unlensed number counts, we find an Einstein radius of (66 per cent confidence limit). This corresponds to a projected velocity dispersion of _v 800 km s¹, in agreement with constraints from strongly lensed features. For a Navarro, Frenk & White mass model, the radial dependence observed indicates a best-fitting halo scalelength of 125 h ¹ kpc. We investigate the uncertainties arising from the observed fluctuations in the unlensed number counts, and show that clustering is the dominant source of error. We extend the maximum-likelihood method to include the effect of incompleteness, and discuss the prospects of further systematic studies of lensing in the near-infrared band.     

Microwave background anisotropies arising from non-linear structures in open and universes

A new method arising from a gauge-theoretic approach to general relativity is applied to the formation of clusters in an expanding universe. The three cosmological models (₀=1, =0), (₀=0.3, =0.7) and (₀=0.3, =0) are considered, which extends our application in two previous papers. A simple initial velocity and density perturbation of finite extent is imposed at the epoch z =1000, and we investigate the subsequent evolution of the density and velocity fields for clusters observed at redshifts z =1, z =2 and z =3. Photon geodesics and redshifts are also calculated so that the cosmic microwave background (CMB) anisotropies arising from collapsing clusters can be estimated. We find that the central CMB temperature decrement is slightly stronger and extends to larger angular scales in the non-zero case. This effect is strongly enhanced in the open case. Gravitational lensing effects are also considered, and we apply our model to the reported microwave decrement observed towards the quasar pair PC 1643+4631 A&B.     

VLA 8.4-GHz monitoring observations of the CLASS gravitational lens B1933+503

The complex 10-component gravitational lens system B1933+503 has been monitored with the Very Large Array (VLA) during the period 1998 February–June with a view to measuring the time delay between the four compact components and hence to determine the Hubble parameter H ₀. Here we present the results of an 'A' configuration 8.4-GHz monitoring campaign that consists of 37 epochs with an average spacing of 2.8 d. The data have yielded light curves for the four flat-spectrum radio components (components 1, 3, 4 and 6). We observe only small flux density changes in the four flat-spectrum components that we do not believe are predominantly intrinsic to the source. Therefore the variations do not allow us to determine the independent time delays in this system. However, the data do allow us to accurately determine the flux density ratios between the four flat-spectrum components. These will prove important as modelling constraints and could prove crucial in future monitoring observations should these data show only a monotonic increase or decrease in the flux densities of the flat-spectrum components.     

海洋中尺度涡旋源汇空间分布特征研究

借助卫星高度计数据,对中尺度涡进行识别和追踪;以16年内中尺度涡个数上的生消为判据,发现中尺度涡在除赤道外的全球大洋中生消频繁,但在海盆内区并没有明显的生成占优区或消亡占优区;而在中纬度近岸的狭窄东边界内中尺度涡生成居多,在另一侧近岸的狭窄西边界中尺度涡消亡居多。同时,我们以一阶斜压模态所对应的特征深度作为两层结构的内界面深度,并假定涡动能平均分配于正压模态和一阶斜压模态,计算得到了包含涡动能和涡有效重力位能的中尺度涡能量年平均净生成率和净耗散率,发现虽然海盆西边界是涡场能量耗散大于能量生成的区域,但强耗散过程实际上在海盆西侧内区的强流及其回流区均有发生。另外,中尺度涡生消个数差值的分布与中尺度涡能量净生成率和净耗散率的分布表明,虽然海盆东边界近岸区域内中尺度涡的生成居多,但该区域中尺度涡的能量偏弱,因此该区并非涡场能量的主要源区。     

重力位三阶梯度张量及其勘探能力初步分析

在重力位三阶梯度张量基本原理的基础上,给出均匀球体重力位零阶至三阶梯度张量的解析表达式,结合理论分析与模型实验,对比各阶梯度张量对场源参数(质量与埋深、水平位置与几何形状)的敏感性。结果表明,重力位三阶梯度张量随场源与观测点之间距离的增大衰减最快。重力曲率张量具有如下特征:对场源埋深变化具有最高的敏感性;对浅部的剩余质量探测能力最强,对深部的剩余质量探测能力最弱;对场源的水平分辨能力及几何形态的区分能力随场源埋深的增大而减小,但重力曲率张量的分辨能力最强;三阶梯度张量的独立元素个数最多,场空间分布形态的类型也最多样,在相同测点分布情况下能够捕获更多的场与场源信息,尤其是重力场的短波成分与浅部的剩余质量。