Reconfiguration and closure of lobe flux by reconnection during northward IMF: possible evidence for signatures in cusp/cleft auroral emissions

Observations are presented of the response of the dayside cusp/cleft aurora to changes in both the clock and elevation angles of the interplanetary magnetic field (IMF) vector, as monitored by the WIND spacecraft. The auroral observations are made in 630 nm light at the winter solstice near magnetic noon, using an all-sky camera and a meridian-scanning photometer on the island of Spitsbergen. The dominant change was the response to a northward turning of the IMF which caused a poleward retreat of the dayside aurora. A second, higher-latitude band of aurora was seen to form following the northward turning, which is interpreted as the effect of lobe reconnection which reconfigures open flux. We suggest that this was made possible in the winter hemisphere, despite the effect of the Earth’s dipole tilt, by a relatively large negative X component of the IMF. A series of five events then formed in the poleward band and these propagated in a southwestward direction and faded at the equatorward edge of the lower-latitude band as it migrated poleward. It is shown that the auroral observations are consistent with overdraped lobe flux being generated by lobe reconnection in the winter hemisphere and subsequently being re-closed by lobe reconnection in the summer hemisphere. We propose that the balance between the reconnection rates at these two sites is modulated by the IMF elevation angle, such that when the IMF points more directly northward, the summer lobe reconnection site dominates, re-closing all overdraped lobe flux and eventually becoming disconnected from the Northern Hemisphere.     

泥沙突变理论在海底管线冲刷中应用

基于泥沙突变理论,针对海底管线冲刷下泥沙的运动特征,建立恒定流作用下的泥沙起动模式,确定希尔兹数、无量纲参数、冲刷坑深度之间相互作用的非线性方程,推导了恒定流作用下海底管线冲刷坑深度的预测公式。将相同条件下该公式的计算结果与前人的试验资料进行了对比,可发现尽管计算结果存在一定的误差,但也基本能满足对冲刷坑深度的预测和判断,从而证明了泥沙突变模型在预测海底管线冲刷坑深度中的适用性。     

磁暴期间极尖区场向电子事件研究

根据Cluster卫星在中高度极尖区的观测数据,分析研究了两次连续磁暴期间极尖区场向电子事件的持续时间以及与Dst值和Dst时间变化率之间的关系.结果表明,磁暴期间场向电子事件的持续时间的范围为6~54 s,大多数场向事件的持续时间小于34 s;极尖区场向电子事件的最大密度和最大场向通量与Dst值没有明显的相关关系;而随着Dst变化率的增加,场向电子最大密度和最大通量也随之增加,场向电子最大密度与Dst变化率之间的相关系数为0.81,场向电子最大通量与Dst变化率之间的相关系数为0.56,下行电子最大通量与Dst变化率之间的相关系数为0.85.经讨论认为行星际磁场持续南向、太阳风速度和动压的急剧增加是引起场向电子通量增加的主要原因.     

基于尖点突变理论的浆砌块石边坡稳定性研究

根据影响浆砌块石挡土墙边坡稳定性的主要控制变量：挡土墙的垂直度i、挡土墙高度h、填料的内摩擦角 、墙后边坡土的重度 、土对挡土墙基底的摩擦系数 、土对挡土墙墙背的摩擦角 等6个因素变量,利用正交设计原理优化试验设计方案,结合库仑理论与力的多边形法,分析计算浆砌块石挡土墙边坡的安全系数,最后用尖点突变理论的突变级数法进一步判断边坡的稳定性。研究结果表明：影响挡土墙边坡稳定性的6个主要控制变量因素的主次关系为 ;在分析挡土墙边坡稳定性时,采用突变级数法进行计算判断,可以直观地判断边坡的稳定情况,从而弥补工程中运用传统的最小安全系数法进行判断出现的模糊不确定的情况。     

相对湿度作用下的石膏矿护顶层突变破坏机制分析

依据室内试验所得的石膏岩的基本力学性质随着大气中相对湿度变化的规律,并结合石膏矿采空区的破坏特征,将护顶层简化为铅直方向受均布荷载q作用的三铰拱分析模型,建立了相对湿度作用下的石膏矿采空区护顶层的尖点突变模型,研究了相对湿度作用下护顶层突发破坏的失稳机制。试验结果表明：石膏岩的力学性质在采空区中环境湿度的作用下,其强度和变形参数会大大降低。分析和工程计算结果表明：随着采空区中环境湿度的增加,支撑体系越不稳定,越容易跨越分叉集而发生突发失稳破坏;相空间的控制参数a随着采空区中环境湿度的增加,其代数值是逐渐增大的（绝对值减小,由负值向0变化）,而控制参数b逐渐增大,系统突发失稳控制参数（a,b）的变化路径为向东北方向变化,该路径是系统较为容易发生突发失稳的路径。     

日侧极光卵的可见光多波段观测特征——中国北极黄河站首次极光观测初步分析

中国在斯瓦尔巴特(Svalbard)群岛新奥尔松(Ny-Alesund)地区建立了一个永久性科学考察站--北极黄河站。北极黄河站(78．92°N,11．93 °E)的修正磁纬为76．24°。2003年11月黄河站建立了一套多波段(427．8nm,557．7nm,630．0nm)单色极光全天空CCD成像观测系统,并于2003年12月11日-2004年2月25日极夜期开展了首次极光越冬观测,获得了1200多小时的连续观测数据。利用这1200多小时观测数据制作了以时间为横轴的南北向极光活动图,对日侧极光卵的极光活动特征进行了研究。初步分析发现,沿日侧极光卵不论磁静日还是磁扰日,在三个波段上都同时观测到了四个重复出现的极光活动区,即0900MLT(磁地方时)附近的 A区、1330MLT的B区和1630MLT的C区以及1200MLT附近的G区。A区内的极光活动由低纬向高纬运动,强度逐渐变弱,形态由较宽的弧状极光向冕状极光演变;B区内的极光活动由高纬向低纬方向运动,形态呈现为冕状极光向较窄的极光弧的演变,极光强度逐渐增强;C区极光活动向高纬方向展宽,强度逐渐变弱,极光由单弧向多重弧演化;而在A与B之间存在一个纬度范围相对较窄的极光活动区G区,该区的极光呈现暗弱的冕状极光。日侧极光活动随时间从午前、正午到午后呈现出一个系统的光谱变化:绿色-红色-绿色。A区的位置出现在卫星探测的午前极光峰之中;而正午附近极光强度暗弱的G区,可部分地解释卫星观测的所谓“正午极光空白区”;卫星观测到的1500MLT附近的“极光热点”区在地面观测中可以区分为以红色极光为主的B区和以绿色极光为主的C区。     

High-time resolution conjugate SuperDARN radar observations of the dayside convection response to changes in IMF B y

We present data from conjugate SuperDARN radars describing the high-latitude ionospheres response to changes in the direction of IMF B_y during a period of steady IMF B_z southward and B_x positive. During this interval, the radars were operating in a special mode which gave high-time resolution data (30 s sampling period) on three adjacent beams with a full scan every 3 min. The location of the radars around magnetic local noon at the time of the event allowed detailed observations of the variations in the ionospheric convection patterns close to the cusp region as IMF B_y varied. A significant time delay was observed in the ionospheric response to the IMF By changes between the two hemispheres. This is explained as being partially a consequence of the location of the dominant merging region on the magnetopause, which is 8/12R_E closer to the northern ionosphere than to the southern ionosphere (along the magnetic field line) due to the dipole tilt of the magnetosphere and the orientation of the IMF. This interpretation supports the anti-parallel merging hypothesis and highlights the importance of the IMF B_x component in solar wind-magnetosphere coupling.     

突变理论在断层活动机理分析中的应用

本文扼要阐明了突变理论的基本思想，介绍了突变理论的Ａ３尖点突变模型。建立了断层运动过程中的势函数，在此基础上，通过对平衡曲面方程的Ｔａｙｌｏｒ级数展开，求取了其标准形式，结合Ｔｈｏｍ的Ａ３类尖点突变，讨论了在不同情况下断层的活动方式。     

Energetic Electrons as a Field Line Topology Tracer in the High Latitude Boundary/CUSP Region: Cluster Rapid Observations

Energetic electrons (e.g., 50 keV) travel along field lines with a high speed of around 20 R_Es⁻¹. These swift electrons trace out field lines in the magnetosphere in a rather short time, and therefore can provide nearly instantaneous information about the changes in the field configuration in regions of geospace. The energetic electrons in the high latitude boundary regions (including the cusp) have been examined in detail by using Cluster/RAPID data for four consecutive high latitude/cusp crossings between 16 March and 19 March 2001. Energetic electrons with high and stable fluxes were observed in the time interval when the IMF had a predominately positive B_z component. These electrons appeared to be associated with a lower plasma density exhibiting no obvious tailward plasma flow (<20 keV). On the other hand, no electrons or only spike-like electron events have been observed in the cusp region during southward IMF. At that time, the plasma density was as high as that in the magnetosheath and was associated with a clear tailward flow. The fact that no stable energetic electron fluxes were observed during southward IMF indicates that the cusp has an open field line geometry. The observations indicate that both the South and North high latitude magnetospheric boundary regions (including both North and South cusp) can be energetic particle trapping regions. The energetic electron observations provide new ways to investigate the dynamic cusp processes. Finally, trajectory tracing of test particles has been performed using the Tsyganenko 96 model; this demonstrates that energetic particles (both ions and electrons) may be indeed trapped in the high latitude magnetosphere.