注水诱发地震的成因及影响因素探讨

根据胜利油田东营凹陷深井注水所监测到的破裂信号特征分析,结合位于同一凹陷内的角7井注水诱发地震特征,对注水诱发地震的成因进行了探讨.注水过程中地层有无先存破裂面对所诱发的地震产生较大影响,认为诱发地震的震级与注采比和注水井的构造位置密切相关.     

大功率激电在鄂拉山口寻找隐伏矿体中的应用

鄂拉山口银多金属矿床位于鄂拉山成矿带东南端,第四系覆盖厚,沼泽发育,存在常年冻土层和碎石流,用常规物探在该区找矿效果不显著.后经大功率激电剖面测量,圈出了具一定规模的激电异常带1条,推断为矿异常,经工程验证,发现隐伏银铅锌矿（化）体多条,说明本区采用大功率激电指导找矿效果显著.     

海盐粒子沉积下碳钢的大气腐蚀初期行为

利用体视显微镜和电化学极化技术原位考察了碳钢上NaCl盐粒的吸潮及其液滴的扩展行为。实验结果表明,NaCl液滴的吸潮水解过程主要受环境相对湿度的影响。相对湿度越高,水解越容易。在极化状态下,NaCl液滴的扩展随极化电流的增加而线性加速。NaCl液滴的扩展与碳钢大气腐蚀的电化学过程相互影响。一方面,NaCl液滴扩展的动力来自于大气腐蚀过程所形成的腐蚀电流,另一方面,NaCl液滴的扩展加大了大气腐蚀过程的阴极面积。进而加速了碳钢的腐蚀过程。     

The instability of the vortex sheet along the shear line

The traditional Kelvin-Helmholtz notion of studying the shear instability is not suitable for the case associated with shear line with the strong wind shear in the vortex sheet. Since then, the shear instability be-comes the instability of the vortex sheet. If the velocity is induced by the vortex sheet, the inequalities (1 – Rv + Rid)> 0 and U (y,t)> U{A(t)} become the criterion of the vortex sheet instability. This criterion indicates that 1) the disposition of environment field restrains the disturbance developing along the shear line. 2) There exist multi-scale interactions in the unstable process of the shear line. The calculation of the necessary condition for the instability is also presented in this paper.     

三分向数据震相的自动识别

利用三分向地震数据,提出了一种自动检测Ｐ波和Ｓ波初至的算法。此算法组合使用了短时窗检测器ＤＳｐ和长时窗ＤＢｐ检测器,具有短时窗的较高精度和长时窗较低的误触发率。应用广东、福建和云南省的地震数据进行测试,结果表明：自动检测具有可靠的精度,地方震和近震Ｐ波到时误差小于０．２ｓ的超过８４％;Ｓ波到时误差小于０．５ｓ的超过７４％。     

Thermal and kinematic corrections to the microwave background polarization induced by galaxy clusters along the line of sight

We derive analytic expressions for the leading-order corrections to the polarization induced in the cosmic microwave background (CMB) owing to scattering of photons off hot electrons in galaxy clusters along the line of sight. For a thermal distribution of electrons with kinetic temperature k _B T _e∼10 keV and bulk peculiar velocity V ∼1000 km s⁻¹, the dominant corrections to the polarization induced by the primordial CMB quadrupole and the cluster peculiar velocity arise from electron thermal motion and are at the level of ∼10 per cent in each case, near the peak of the polarization signal. When more sensitive measurements become feasible, these effects will be significant for the determination of transverse peculiar velocities, and the value of the CMB quadrupole at the cluster redshift, via the cluster polarization route.     

The optical polarization of spiral galaxies

Scattering of starlight by dust, molecules and electrons in spiral galaxies will produce a modification of the direct intensity and a polarization in the observed light. We treat the case where the distribution of scatterers can be considered to be optically thin, and derive semi-analytic expressions for the resolved intensity and polarized intensity for Thomson, Rayleigh, and more general scattering mechanisms. These expressions are applied to a parametric model for spiral galaxies. It is further shown that in the case of Thomson and Rayleigh scattering, and when scatterers and stars are distributed with rotational symmetry, the total polarized flux depends on the inclination, i , of the galactic axis to the line of sight according to a simple sin²  i law. This generalizes the well-known result for point-like and spherical light sources. By using a method based on spherical harmonics, we generalize this law for more general mechanisms, and show that to good approximation, the sin²  i law still holds for the class of models considered.     

A generic scattering model for AGN

I present a development of the scattering model of Young et al. that can reproduce the velocity resolved polarization of the scattered broad lines, along with the continuum polarization of AGN. Two possible emission models are presented, namely a rotating disc and a radially expanding shell of emission. Using known, or expected, scattering regions present in AGN it is possible to reproduce the polarization observed to be present in type 1 and type 2 active galaxies.
The use of the model is illustrated by its application of the spectropolarimetric observations of the Seyfert 1 galaxy, Mrk 509. By a simple alteration of the incident flux upon the scattering regions it is shown that the time variable polarization in this object can be reproduced.