水库诱震机制新理论的探索──断层带弱化与岩体软化效应诱震理论

针对走滑断层诱发的水库地震，建立了尖点突变模型，提出了发震的充要力学条件判据及地震释放能量的简单表达式。以突变理论分析为依据，建立了水库诱震机制的新假说，简称为断层带弱化与岩体软化效应诱震理论，较合理地解释了水库地震与岩性、构造、水位的关系及水库地震序列ｂ值的特征。本文的讨论从整体上深化了对水库诱震机制的认识。     

极隙区粒子和电流的观测和研究

处于高纬向日面的极隙区是太阳风能量、动量和质量可以直接进入地球磁场并到达地球的近地空间的区域。本文简要介绍了极隙区的观测和研究，综述了极隙区的粒子沉降、场向电流、等离子体对流和电离层电流的特征。     

滑坡演化的非线性动力学与突变分析

基于对任-连续函数, 至少在较小的邻域内可以用多项式任意逼近的数学理论, 运用改进的Backus广义线性反演理论, 以斜坡位移时间序列为基础, 反演建立了斜坡演化的非线性动力学模型。并利用自治梯度系统与突变模型的等价性, 通过变量代换得到标准的尖点突变模型。以黄茨及卧龙寺滑坡为例对滑坡的发展孕育过程进行分析, 结果表明:该非线性动力学模型不仅预测效果十分理想, 而且具有较高的自我调整适应能力; 斜坡临滑前都以突变特征值D的突降至零为前兆特征, 可作为-个具有物理意义的前兆指标。     

煤柱-顶板系统协同作用的脆性失稳与非线性演化机制

把坚硬顶板视为弹性梁,把煤柱视为应变软化介质并采用W e ibu ll分布描述它的损伤本构模型,本文对坚硬顶板和煤柱组成的力学系统,用突变理论方法研究了它的演化失稳过程。通过对建立的尖点突变模型的分析发现,系统失稳主要取决于系统的刚度比k与材料的均匀性或脆性指标m值,并给出了失稳的充要条件力学判据和失稳突跳量的表达式。考虑煤柱介质的粘性或蠕变性,建立了系统演化的非线性动力学模型物理预报模型,并给出了根据顶板沉降观测数据反演非线性动力学模型的方法和稳定性判别准则。对木城涧矿根据观测序列进行了动力学模型的反演分析,一个重要发现是:D值在临近失稳时陡增出现峰值而后急剧下降。根据材料损伤与声发射累计计数的对应关系,建立了系统演化过程中声发射率的动力学模型,并进行了声发射模拟分析和分维分析,发现m值与系统的演化路径对系统演化的声发射活动规律及分维特征有重要影响,单纯根据声发射监测和降维现象预报冲击地压是不可靠的。     

Interball contribution to the high-altitude cusp observations

The polar cusps have traditionally been described as narrow funnel-shaped regions of magnetospheric magnetic field lines directly connected to magnetosheath, allowing the magnetosheath plasma to precipitate into the ionosphere. However, recent observations and theoretical considerations revealed that the formation of the cusp cannot be treated separately from the processes along the whole dayside magnetopause and that the plasma in regions like cleft or low-latitude boundary layer is of the same origin. Our review of statistical results as well as numerous case studies identified the anti-parallel merging at the magnetopause as the principal source of the magnetosheath plasma in all altitudes. Since effective merging requires a low plasma speed at the reconnection spot, we have found that the magnetopause shape and especially its indentation at the outer cusp is a very important part of the whole process. The plasma is slowed down in this indentation and arising multiscale turbulent processes enhance the reconnection rate.     

高密度极尖区的形成原因

极尖区是太阳风进入磁层的一个重要窗口,极尖区密度是反映这一物理过程的重要参量,通常情况下极尖区密度约为1~10 cm^-3,但有时卫星会观测到密度大于40 cm^-3的极尖区,本文称之为高密度极尖区.我们分析了Cluster卫星2001—2009年的观测数据,在470个极尖区穿越中找到28个高密度极尖区穿越事件并进行了统计研究,分析了高密度极尖区事件的形成原因,进而讨论了太阳风高效地进入极尖区的外部条件.结果表明：距正午的距离（｜MLT-12｜）较小,太阳风的密度高,低纬有磁层顶磁重联发生以及正偶极倾角都是观测到高密度极尖区事件的有利条件,并且当同时满足上述4个条件时,高密度极尖区事件发生率为100%;而低纬磁层顶磁重联以及大的正偶极倾角被认为是太阳风高效地进入极尖区的重要条件.这些研究结果有助于我们更进一步地理解太阳风进入极尖区的物理机制.     

极隙区场向电流对高纬电离层电场和电流体系的影响

用Ｋａｍｉｄｅ－Ｍａｔｓｕｓｈｉｔａ方法，在行星际磁场具有较小的北向分量，且｜Ｂｙ｜＞＞｜Ｂｋ｜时，对磁语和磁扰状态以及Ｂｒ＞０和Ｂｙ＜０等不同情况，分别计算了场向电流引起的电离层电势、电场和电流体系．结果表明，极隙区场向电流的存在使高纬向日面区域的电势发生畸变，当Ｂｙ＞０时，无论是磁扰还是磁静日，极隙区电场具有显著的北向分量；等离子体对流有较大的西向分量；电离层电流为东向电流．当Ｂｙ＜０时，电场和等离子体对流的方向与Ｂｙ＞０时相反；电离层电流在磁抗日有西向分量，但在磁静日没有西向分量．电导率对电场和电流体系的影响十分明显，磁扰极光带电导率增强使电流涡从背阳面向向阳而漂移，与静日相比，磁扰时极隙区场向电流引起的电场畸变更为明显，但电场和电流强度的大小却基本保持不变．     

Pc3–4 ULF waves at polar latitudes

A search for Pc3–4 wave activity was performed using data from a trans-Antarctic profile of search-coil magnetometers extending from the auroral zone through cusp latitudes and deep into the polar cap. Pc3–4 pulsations were found to be a ubiquitous element of ULF wave activity in all these regions. The diurnal variations of Pc3 and Pc4 pulsations at different latitudes have been statistically examined using discrimination between wave packets (pulsations) and noise. Daily variations of the Pc3–4 wave power differ for the stations at the polar cap, cusp, and auroral latitudes, which suggests the occurrence of several channels of propagation of upstream wave energy to the ground: via the equatorial magnetosphere, cusp, and lobe/mantle. An additional maximum of Pc3 pulsations during early-morning hours in the polar cap has been detected. This maximum, possibly, is due to the proximity of the geomagnetic field lines at these hours to the exterior cusp. The statistical relation between the occurrence of Pc3–4 pulsations and interplanetary parameters has been examined by analyzing normalized distributions of wave occurrence probability. The dependences of the occurrence probability of Pc3–4 pulsations on the IMF and solar wind parameters are nearly the same at all latitudes, but remarkably different for the Pc3 and Pc4 bands. We conclude that the mechanisms of high-latitude Pc3 and Pc4 pulsations are different: Pc3 waves are generated in the foreshock upstream of the quasi-parallel bow shock, whereas the source of the Pc4 activity is related to magnetospheric activity. Hourly Pc3 power has been found to be strongly dependent on the season: the power ratio between the polar summer and winter seasons is 8. The effect of substantial suppression of the Pc3 amplitudes during the polar night is reasonably well explained by the features of Alfven wave transmission through the ionosphere. Spectral analysis of the daily energy of Pc3 and Pc4 pulsations in the polar cap revealed the occurrence of several periodicities. Periodic modulations with periods 26, 13 and 8–9 days are caused by similar periodicities in the solar wind and IMF parameters, whereas the 18-day periodicity, observed during the polar winter only, is caused, probably, by modulation of the ionospheric conductance by atmospheric planetary waves. The occurrence of the narrow-band Pc3 waves in the polar cap is a challenge to modelers, because so far no band-pass filtering mechanism on open field lines has been identified.     

Magnetopause stand-off distance in dependence on the magnetosheath and solar wind parameters

A model of the magnetosheath structure proposed in a recent paper from the authors is extended to estimate the magnetopause stand-off distance from solar wind data. For this purpose, the relationship of the magnetopause location to the magnetosheath and solar wind parameters is studied. It is shown that magnetopause erosion may be explained in terms of the magnetosheath magnetic field penetration into the magnetosphere. The coefficient of penetration (the ratio of the magnetospheric magnetic field depression to the intensity of the magnetosheath magnetic field B_mz = -B_m sin²/2, is estimated and found approximately to equal 1. It is shown that having combined a magnetosheath model presented in an earlier paper and the magnetosheath field penetration model presented in this paper, it is possible to predict the magnetopause stand-off distance from solar wind parameters.     

Effects of density, temperature and velocity gradients on inertial Alfven wave in cusp region

The kinetic approach is used to evaluate the dispersion relation and growth/damping rate of inertial Alfven wave (IAW) with density, temperature and velocity gradients in an inhomogeneous plasma. The effects of gradient terms are studied for both the regions k_⊥ρ_i<1 and k_⊥ρ_i>1, where k_⊥ is the perpendicular wave number and ρ_i is the ion gyroradius. The relevance of theoretical results so obtained is predicted in accordance to the FAST observations in the cusp region. The results are interpreted for the space plasma parameters appropriate to the cusp region. This study elucidates a possible scenario to account for the particle acceleration and the wave dissipation in inhomogeneous plasmas. This model is also able to explain many features observed in plasma sheet boundary layer as well as to evaluate the dispersion relation, growth/damping rate and growth/damping length of inertial Alfven wave. It is found that density, temperature and velocity gradients control the wave frequency and effectively enhance the growth rate of inertial Alfven wave.