2000年7月重大太阳事件的极隙区纬度观测研究

20 0 0年 7月 ,太阳表面发生了一系列的耀斑与日冕物质抛射事件 ,最大耀斑能级达X5 .7/3 B。地球表面发生相应特大磁暴 ,Dst指数最大负偏达 - 3 0 0 n T。中国南极中山站地处极隙区纬度 ,白天位于磁层极隙区 ,夜间位于极盖区 ,以多种高空大气物理观测设备详细记录了该磁暴过程。对有关数据的分析表明 ,高能粒子引起电离层吸收急剧增加 ,测高仪数据两天多信号空白 ,宇宙噪声吸收显著增加 ;地磁 Pc3 /5脉动增加与行星际磁场南向分量密切对应 ,显示行星际磁流体波对激发磁层脉动的贡献 ;磁暴主相期间 ,Pc3 /5脉动大幅度增加 ;极区地磁水平分量随南向行星际磁场变化 ,但滞后近 8小时 ;Dst指数与南向行星际磁场密切相关 ,磁暴受控于高度负偏的南向行星际磁场     

Radio Tomography: A New Experimental Technique

The technique of radio tomography has developed during the past fifteen years from a theoretical concept to an established experimental method, used for geophysical investigations ofsolar-terrestrial processes. It also has potential in the mapping and modelling of the ionised atmosphere for application to practical radio systems. The method involves measurement of the electron content of the ionosphere along a large number of intersecting satellite-to-receiver ray paths, with tomographic inversion of the data to give a two-dimensional image of the spatial distribution of plasma density in the region of ray-path intersection. The emphasis in this review is on experimental tomographic observations, which have highlighted the capabilities and potential of the technique. Examples are presented from the equatorial sector where the equatorial anomaly is a significant feature, the mid-latitude sector where radio propagation is often influenced by the presence of the main ionisation trough, and the auroral and polar regions where footprints of solar-terrestrial coupling processes are frequently to be seen.     

极隙区纬度太阳活动高年背景电离层特征

本文利用 EISCAT-Svalbard 雷达1999年3月至2003年2月期间观测数据,对太阳活动高年前后极区电离层 F 区电子密度随高度和地方时的二维分布进行统计分析,研究极隙/极盖区背景电离层特征,并与 IRI-2001模式预测结果进行比较。分析结果表明,在 ESR 雷达所在纬度,不存在“冬季异常”现象;但首次发现,此处电离层冬季日变化存在磁午夜前主极大。另外,无论在什么季节,白天时段 ESR 雷达上空电子密度都在磁正午附近有一极大值。与 IRI 模式的比较表明,模式预测的 F 区电子密度与 ESR 实测结果存在较大偏差,在500km 高度以上的顶部电离层和冬季,差别尤其明显。简要讨论了软粒子沉降对造成电子密度日变化磁正午极大的作用和冬季磁午夜前主极大的形成机理。     

Cusp Modeling and Observations at Low Altitude

Cusp properties have been investigated with an open-field line particle precipitation model and Defense Meteorological Satellite Program (DMSP) satellite observations. Particular emphasis is placed on the effects of IMF B_y, since previous studies focus mostly on IMF B_z. The model-data comparisons for various IMF configurations show that the model captures the large-scale features of the particle precipitation very well, not only in the cusp region, but also in other open-field line regions such as the mantle, polar rain, and open-field line low-altitude boundary layer (LLBL). When the IMF is strongly duskward/dawnward and weakly southward, the model predicts the occurrence of double cusp near noon: one cusp at lower latitude and one at higher latitude. The lower latitude cusp ions originate from the low-latitude magnetosheath whereas the higher latitude ions originate from the high-latitude magnetosheath. The lower latitude cusp is located in the region of weak azimuthal E × B drift, resulting in a dispersionless cusp. The higher latitude cusp is located in the region of strong azimuthal and poleward E × B drift. Because of a significant poleward drift, the higher latitude cusp dispersion has some resemblance to that of the typical southward IMF cusp. Occasionally, the two parts of the double cusp have such narrow latitudinal separation that they give the appearance of just one cusp with extended latitudinal width. From the 40 DMSP passes selected during periods of large (positive or negative) IMF B_y and small negative IMF B_z, 30 (75%) of the passes exhibit double cusps or cusps with extended latitudinal width. The double cusp result is consistent with the following statistical results: (1) the cusp’s latitudinal width increases with |IMF B_y| and (2) the cusp’s equatorward boundary moves to lower latitude with increasing |IMF B_y|.     

考虑围岩流变特性的地震尖点型突变模型

考虑到断层两盘围岩的粘弹性和断层的应变弱化,建立了断层地震的简化力学模型,首先证明了该模型对应于尖点突变,后利用尖点突变理论研究地震的非稳定机制,阐明只有当外界对系统输入足够的能量,且刚度比小于１时,系统内的能量才能迅地转移与释放,引起地震。而孕震时间既与远场位 关又与围岩的粘弹性性质有关。     

突变理论在层状岩体破碎分析中的应用

本文简要介绍突变理论的尖点突变模型。在分析层状岩体在爆炸冲击荷载作用下破碎程度主要受控因素的基础上,运用拟合的途径建立了岩石破碎分析的尖点突变控制方程。该方程可以被用来直接定量计算岩石破碎块度发生明显变化点的炸药单耗(q)或炮孔与层状结构面间的夹角(α),实践证明是可行的。     

地震作用下岩羊村滑坡稳定性与失稳机制研究

以云南香丽高速公路沿线的岩羊村滑坡为研究对象,开展了滑坡动力稳定性评价及失稳机制研究：进行了不同烈度地震下的滑坡稳定性分析,采用滑带弹性区体积占比的变化反映其失稳过程,结合滑坡变形破坏模式,对滑坡整体稳定性进行评价;针对极限地震工况,分别从时间和空间角度描述滑坡失稳过程;建立了同时考虑滑带弱化和硬化的滑坡尖点突变模型,揭示了滑坡失稳的触发机制。研究表明：滑坡在区域Ⅷ度地震烈度条件下基本保持稳定,在锁固段的“锁固作用”下滑坡仅发生局部破坏;滑坡发生整体失稳的临界峰值加速度为2.29 m/s2,其失稳机制为在前缘牵引、后缘拉裂作用下,滑带塑性区贯通导致的整体失稳;地震作用下滑带前缘、中部、后缘并非同步破坏,表现为累积?触发效应;利用改进尖点突变模型推导了刚度效应失稳判据,揭示了滑坡整体稳定性与滑带介质的刚度及尺寸特性密切相关。研究结果为岩羊村滑坡的防治与抗震设计提供了指导,并可为同类工程的动力稳定性评价与失稳机制分析所借鉴。     

基于尖点突变理论及非趋势波动分析的滑坡稳定性及变形特征研究

以尖点突变理论及非趋势波动分析为基础,构建滑坡稳定性及变形趋势判断模型。首先利用尖点突变理论对滑坡整体稳定性进行评价,并进一步探讨滑坡的分阶段稳定性特征;再利用非趋势波动分析判断滑坡累计序列和速率序列的整体及分阶段变形趋势,并与稳定性分析结果进行对比。实例表明,两种分析方法的结果具有较好的一致性。在分阶段研究中,等时段和递增时段的分析结果具有明显差异,说明阶段分解方式对结果的影响较大,且以递增时段分析结果的规律性更强。     

Magnetopause boundary structure deduced from the high-time resolution particle experiment on the Equator-S spacecraft

An electrostatic analyser (ESA) onboard the Equator-S spacecraft operating in coordination with a potential control device (PCD) has obtained the first accurate electron energy spectrum with energies &7 eV-100 eV in the vicinity of the magnetopause. On 8 January, 1998, a solar wind pressure increase pushed the magnetopause inward, leaving the Equator-S spacecraft in the magnetosheath. On the return into the magnetosphere approximately 80 min later, the magnetopause was observed by the ESA and the solid state telescopes (the SSTs detected electrons and ions with energies &20–300 keV). The high time resolution (3 s) data from ESA and SST show the boundary region contains of multiple plasma sources that appear to evolve in space and time. We show that electrons with energies &7 eV–100 eV permeate the outer regions of the magnetosphere, from the magnetopause to &6Re. Pitch-angle distributions of &20–300 keV electrons show the electrons travel in both directions along the magnetic field with a peak at 90° indicating a trapped configuration. The IMF during this interval was dominated by Bx and By components with a small Bz.     

Identification of magnetosheath mirror modes in Equator-S magnetic field data

Between December 1997 and March 1998 Equator-S made a number of excursions into the dawn-side magnetosheath, over a range of local times between 6:00 and 10:40 LT. Clear mirror-like structures, characterised by compressive fluctuations in |B| on occasion lasting for up to 5 h, were observed during a significant fraction of these orbits. During most of these passes the satellite appeared to remain close to the magnetopause (within 1–2 Re), during sustained compressions of the magnetosphere, and so the characteristics of the mirror structures are used as a diagnostic of magnetosheath structure close to the magnetopause during these orbits. It is found that in the majority of cases mirror-like activity persists, undamped, to within a few minutes of the magnetopause, with no observable ramp in |B|, irrespective of the magnetic shear across the boundary. This suggests that any plasma depletion layer is typically of narrow extent or absent at the location of the satellite, at least during the subset of orbits containing strong magnetosheath mirror-mode signatures. Power spectra for the mirror signatures show predominately field aligned power, a well defined shoulder at around 3–10 × 10⁻² Hz and decreasing power at higher frequencies. On occasions the fluctuations are more sinusoidal, leading to peaked spectra instead of a shoulder. In all cases mirror structures are found to lie approximately parallel to the observed magnetopause boundary. There is some indication that the amplitude of the compressional fluctuations tends to be greater closer to the magnetopause. This has not been previously reported in the Earth’s magnetosphere, but has been suggested in the case of other planets.