高纬磁层顶尾部边界层的离子流剪切不稳定性

研究了高纬磁层顶层部边界层在非均匀磁场条件下的离子流剪切不稳定性,由于考虑了尾向电流,我们发现离子流剪切不稳定性的激发与扰动波长有关,并得到了激发该不稳定性的准临界波长的表达式,对于磁层顶存在的波长为地球半径量级的表面波扰动,离子流剪切不稳定性倾向于发生在磁层顶边界层的内边界,沿磁层顶外边界传播的稳定的表面波和其内边界的离子流剪切不稳定性同时存在,这将有助于解释磁鞘太阳与动量持续不断地向地磁层的传输。     

磁层顶剪切磁流体非线性性态的谱截断法研究Ⅰ.流场扰动对磁场的作用

本文用谱截断方法研究了磁层顶剪切磁流体的非线性性态。结果表明:流场扰动会使系统出现剪切不稳定(K-H不稳定)性;系统具有对初值的敏感性,这是导致湍动而使磁层顶动力学性态难以预测的根本原因;流场粘性及流场与磁场的相互作用使能量与动量在流场与磁场中转化和传输;外界能流通过粘性与耦合作用可周而复始地在系统中传递。     

远磁尾磁层顶位形的偏转

利用WIND和ARTEMIS卫星观测数据,分析远磁尾磁层顶对行星际和太阳风变化的响应,尤其是偏离日地连线的太阳风速度改变对远磁尾磁层顶的影响.研究发现在2011年9月13日的事件中,P2卫星观测到高速且高密度的磁鞘流.利用最小变量法进行分析发现,磁层顶沿着偏离日地连线的太阳风速度方向发生偏转.根据相似三角形定理,推断出本次事件中磁层顶在y方向和z方向上的偏转幅度分别达到10R_e和6R_e.P1和P2卫星的相对位置也证实了这一观点.因此,偏离日地连线的太阳风速度对远磁尾磁层顶的位形影响很大.研究结果可为建立包含太阳风速度v_y和v_z效应的磁层顶模型提供观测证据.     

磁鞘快速流引起的磁层顶凹陷事件

最近研究表叽磁层顶凹陷对磁层-电离层耦合具有重要作用.但是,磁层顶凹陷现象的确认需要多颗卫星的联合观测,目前为止报道的磁层顶凹陷事例非常少.本文利用THEMIS 5颗卫星的联合观测结果,分析了一例由磁鞘快速流引起的磁层顶凹陷事件.2007年7月21日10:00UT-10:45UT,位于日下点磁层顶附近的THEMIS卫星...     

磁层顶穿越事件自动识别算法

磁层顶是太阳风与磁层进行质量、动量、能量交换的关键区域.磁层顶穿越事件（MCEs）可通过对卫星探测到的粒子能谱和磁场数据图进行人工分析的方式来识别.因太阳风动压和行星际磁场的易变性,位于磁层顶附近的卫星经过长期观测可能会经历成千上万次的磁层顶穿越.人工分析的方法工作量巨大,而且识别速度慢.本文发展了一种新的日下点附近MCEs自动识别算法.此算法综合分析卫星探测到的粒子和磁场数据,能有效地减少误判的发生.为了验证算法的有效性,采用单CPU计算机对THEMIS卫星在2007—2018年靠近日下点附近观测到的数据进行MCEs自动识别,最终在约6h共识别出16758个MCEs.这些自动识别出来的MCEs样本可用于统计研究磁层顶相关的诸多物理问题,如凹陷磁层顶、太阳风与磁层相互作用,磁层顶磁场重联等.同时还分析了算法的精确性和局限性.     

基于MHD模拟数据的正午午夜子午面磁层顶位形研究

通过分析太阳风-磁层-电离层系统的三维全球磁流体力学(MHD)模型的计算数据, 给出了正午-午夜子午面磁层顶位形的定量模型. 分析表明, 正午-午夜子午面磁层顶位形可以用文献[3]提出的基于卫星观测数据的、描述赤道面磁层顶位形的函数来描述. 与赤道面磁层顶不同, 正午-午夜子午面磁层顶位形更为复杂. 在忽略极尖区(cusp)的简化条件下, 磁层顶位形仍需利用两条曲线来拟合. 太阳风动压Dp与行星际磁场分量Bz是控制磁层顶位形的主要因素. 行星际磁场为北向时, 磁场增强, 日下点距离r0增大; 行星际磁场为南向时, 磁场增强, 磁层顶日下点距离r0减小. 整体而言, 行星际磁场分量Bz由南转北时, r0增大, 且Bz对r0的影响减弱. 太阳风动压Dp是控制磁层顶日下点的主要因素, Dp增大, r0减小. 磁层顶位形的另一个参数磁层顶磁尾张角α, 随着行星际磁场南向分量增强而增大, 即磁层顶张开程度更加显著, 更多的磁通量由向阳侧传输到夜侧; Dp增大, α略增大, 这意味着Dp对磁通量由日侧向夜侧的传输也有一定的贡献.     

火星磁层顶形成和变化的理论研究

考虑太阳风动压与行星电离层中的带电粒子热压及磁压之和平衡,建立了有大气（电离层）的行星磁层顶形成的理论模型,结合卫星对火星的观测数据,对子午面内向日侧火星磁层顶位形进行了数值计算和分析,研究了火星磁层顶位形及其与太阳风动压之间的变化关系．结果认为,火星磁层顶位形与地球磁层顶相似．太阳风动压越大,火星磁层顶越靠近火星;太阳风动压越弱,火星磁层顶越远离火星．根据火星内秉磁矩从古到今逐渐减小的观点,探索了大尺度磁场（内禀磁矩）对火星磁层顶的贡献作用,结果认为大尺度磁场越强,火星磁层顶越远离行星．这对于进一步研究火星磁层的长期演化以及其他行星磁层的位形变化都具有重要的意义．     

磁层顶通量传输事件轴向统计分析

磁层顶通量传输事件（Flux Transfer Event,FTE）与磁重联相关,其典型特征为磁场法向分量的双极变化.在不同FTE模型里,FTE结构可能为重联的通量管、由多X线重联形成的闭合磁通量绳或者由单X线重联形成的开放磁场环,从而在磁层顶有不同的整体位形.使用一种新的轴向分析方法,对Cluster在一个向阳面磁层顶穿越季观测到的505个FTE进行统计研究.结果表明：在磁层顶中低纬度的侧翼,大多数FTE轴向均为沿磁层磁力线方向即南北方向,少数FTE轴向沿着不同于磁层磁力线方向的东西方向;在高纬磁层顶,大多数FTE轴向沿东西方向,少数FTE轴向沿着磁层磁力线方向即南北方向.这些统计特征有助于重新认识FTE的全球形态.     

Forecasting magnetopause crossing locations by using Neural Networks

Given the highly complex and nonlinear nature of Near Earth Space processes, mathematical modeling of these processes is usually difficult or impossible. In such cases, modeling methods involving Artificial Intelligence may be employed. We demonstrate that data driven models, such as the Neural Network based approach, shows promise in its ability to forecast or predict the behavior of these processes. In this paper, modeling studies for forecasting magnetopause crossing locations are summarized and a Neural Network algorithm is presented to describe the nonlinear time-dependent response of the subsolar region of the magnetopause to varying solar wind conditions. In our approach the past history of the solar wind has, for the first time to the best knowledge of the authors, been included in forecasting the subsolar region of the magnetopause. It is proposed that the data driven approach is a valid approach to understanding and modeling the physical phenomena of Near Earth Space. The only basic requirement for the data driven approach is the availability of representative data for the phenomena. The objective of this paper is to demonstrate that by using WIND and GEOTAIL satellite data a Neural Network based model can be adapted to the modeling of the Earth’s magnetopause.     

Long period magnetospheric oscillations at discrete frequencies: The results of a multi-station analysis

A multi-station analysis of geomagnetic field measurements conducted for a remarkable case event, at a European and an American array shows that, although several aspects of the geomagnetic field observations show a clear latitudinal and local time dependence, simultaneous oscillations at discrete frequencies (f ≈ 1.0, 1.3, 2.2 and 3.2 mHz) are almost ubiquitously detected, from low to high latitudes both in the light and dark sector. They are driven by fluctuations of the solar wind density and dynamic pressure at the same frequencies, via the modulation of the magnetopause current. We also report clear evidence for the occurrence of resonant coupling (at f ≈ 2.2 and 3.2 mHz) between such modes and high latitude field lines. Due to the variable length of the field line through the day, oscillation modes at the same frequencies resonate at different latitudes in the daytime and nighttime region, respectively.     

A Theoretic Interpretation of Movement of the Cusp Equatorward Boundary

A preliminary model is proposed to describe quantitatively the position and movement of cusp equatorward boundary. This integrated model, consisting of an empirical model of the magnetopause and a compressed dipolar model of Open/Closed field line, connects quantitatively the solar wind conditions, subsolar magnetopause and cusp equatorward boundary. It is shown that the increasing solar wind dynamic pressure and the increasing southward Interplanetary Magnetic Field (IMF) component drive the magnetopause to move inward and the cusp equatorward. This model is adopted to interpret quantitatively the cusp movement of August 14, 2001 observed by Cluster. The results show that the subsolar magnetopause moved earthward from 10.7 He to 9.0 Re during the period of 002300-002800 UT, and correspondingly the cusp equatorward boundary shifted equatorward. The observations of Cluster C1 and C4 show the cusp equatorward boundary that Cluster Cl and C4 were crossing during same interval moved equatorward by 4.6°. The cusp equatorward boundary velocity computed in the theoretical model (10.7km/s) is in good agreement with the observed value (9.4km/s) calculated from the data of CIS of Cluster C4 and C1.     

Comparison of the magnetic field before the subsolar magnetopause with the magnetic field in the solar wind before the bow shock

Crossings of the magnetopause near the subsolar point are analyzed using data of THEMIS mission. Variations of the magnetic field near magnetopause measured by one of THEMIS satellites are studied and compared with simultaneous measurements in the solar wind by another THEMIS satellite. The time delay of the solar wind arrival at the subsolar point of the magnetopause is taken into account. 30 and 90 s averaging of the magnetic field in the magnetosheath is produced. The results of averaging are compared with the results of measurements in the solar wind before the bow shock and foreshock. It is shown, that _Bx$B_x$ component of the magnetic field near magnetopause is near to zero, which supports the possibility to consider the magnetopause as the tangential discontinuity. Comparatively good correlation of _By$B_y$ component in the solar wind and near the magnetopause is observed. The correlation of _Bz$B_z$ component near the magnetopause and IMF is practically absent, the sign of the _Bz$B_z$ near the subsolar point does not coincide with the sign of IMF _Bz$B_z$ in ∼$\sim$30% cases.     

行星际磁场北向时磁层顶区磁场重联的全球模式

在对背阳面磁层顶区局域磁场重联模拟的基础上提出了一个行星际磁场北向时磁层顶磁场重联的全球模式。行星际磁场北向时碰层顶磁场重联导致近地尾瓣的能量被输送到远磁尾,太阳风能量不在磁尾储存,向阳面磁层顶变厚,磁层受到一系列扰动。