|
|
|
题名
|
作者
|
年代
|
出处
|
被引量
|
| 1 | MHD and kinetic analysis of flow bursts in the Earth's plasma sheet显示文摘In an attempt to study the flow bursts in the Earth’s plasma sheet we select an event that took place on August 7,2004 in the expansion phase of a substorm,using data from the geomagnetic index,solar wind data,plasma and magnetic field observations from C1 Cluster satellite(the Cluster mission has 4 satellites)and from Double Star TC-1 satellite.In MHD approach,TC-1 firstly observed the tailward flow,then the earthward,and finally the flow alternated in two directions.C1 firstly observed the earthward plasma flow,and then the tailward plasma flow.Before flow bursts are observed by TC-1 and C1,there are disturbances in local entropy with their tailward local entropy larger than those of the earthward.The kinetic features of the plasma flow observed by C1 are similar to those in MHD.However,kinetic characteristics of the plasma flow observed by TC-1 are far more than the description in MHD.The inadequacy mainly exists in two cases:(i)the firstly enhanced tailward flows given in MHD are found without significant increase of the energetic tailward flux;(ii)the almost stagnant flow in MHD is composed of the enhanced energetic ion flux in both earthward and tailward directions.The earthward flow burst observed by TC-1 might be multiple overshoots and rebounds.The earthward flow burst observed by C1 might be simply rebounded in the near-Earth.The pulsation observed by C1 is earlier than that observed by TC-1 with the former intensity less than that of the latter.After the energetic ion flux in the tailward direction is significantly enhanced,the power spectrum intensity of the ULF wave commences to increase obviously,which may suggest that the stream instability is closely correlated with ULF pulsations. | MA YuDuan CAO JinBin FU HuiShan REME H. DANDOURAS I. YANG JunYing WANG ZhiQiang TAO Dan YANG Jian | 2014 | Science China(Technological Sciences)2014，57，1： | 7 |
| 2 | Convective high-speed flow and field-aligned high-speed flows explored by TC-1显示文摘From June 1, 2004 to October 31, 2006, a total 465 high-speed flow events are observed by the TC-1 satellite in the near-Earth region (?13 RE < x < ?9 RE, |Y |<10 RE, |Z|<5 RE). Based on the angle between the flow and the magnetic field, the high-speed flow events are further divided into two types, that is, field-aligned high-speed flow (FAHF) in the plasma sheet boundary and convective bursty bulk flow (BBF) in the center plasma sheet. Among the total 465 high-speed flow events, there are 371 FAHFs, and 94 BBFs. The CHF are mainly concentrated in the plasma sheet, the intersection angle between the flow and the magnetic field is larger, the magnetic field intensity is relatively weak. The FHF are mainly distributed near the boundary layer of the plasma sheet, the intersection angle between the flow and magnetic field is smaller, and the magnetic field intensity is relatively strong. The convective BBFs have an important effect on the substorm. | ZHANG LingQian LIU ZhenXing MA ZhiWei W. BAUMJOHANN M.W. DUNLOP WANG GuangJun WANG Xiao H. REME C. CARR | 2008 | Chinese Science Bulletin2008，53，15： | 5 |
| 3 | 一次磁层亚暴期间磁场偶极化的尾向传播显示文摘利用TC1、Cluster和Polar结合极光和同步高度及地磁的观测,研究了2004年9月14日1730~1930UT时间段的亚暴偶极化过程.此前行星际磁场持续南向几个小时.亚暴初发(Onset)开始于1823UT.2min之后,同步高度的LANL-02A在子夜附近观测到了明显的能量电子增强(Injection)事件,而TC1在1827UT左右在磁尾(-10,-2,0)RE(GSE)观测到了磁场BX的突然下降,伴随着等离子体压强和温度的突然增加及磁场的强烈扰动.在(-16,1,3)RE(GSE)的Cluster上相同的仪器观测到相同的现象,只是比TC1观测到的晚大约23min,在1850UT左右.虽然Polar在更靠近地球的较高纬度(-7.5,3.5,-4.0)RE(GSE)附近,也在1855UT左右观测到了这种磁场偶极化现象.以上的观测时序表明TC1、Cluster观测到的磁场偶极化比亚暴偶极化初始发生分别晚4min和27min.说明偶极化由近磁尾向中磁尾传播.详细计算表明偶极化源区的位置大约在X=-7.7RE~-8.6RE,而传播速度大约为70km.s-1.在这个事件中亚暴的物理图像可能是中磁尾的近地重联产生的地向高速流到达近磁尾,为近磁尾的亚暴触发创造了条件;亚暴在近磁尾触发之后,磁场偶极化峰面向中磁尾传播. | 曹馨 濮祖荫 张辉 傅绥燕 马志伟 肖池阶 刘振兴 谢伦 Dunlpo M.W. Korth A. Frazen M. Zong Q.G. Lueck E. Carr C. Reme H. Glassmeier K.H. | 2007 | 地球物理学报2007，50，4： | 3 |
| 4 | The correlations of ions density with geomagnetic activity and solar dynamic pressure in cusp region显示文摘A statistical study of the properties of ions (O+, He+ and H+) measured by the Cluster-II in cusp region as a function of the solar wind dynamic pressure and geomagnetic index Kp respectively was made dur-ing the summer and fall of 2001-2003. The main results are that: (1) O+ ion density responds in a sig-nificant way to geomagnetic index Kp, and He+ ion density is not correlated with geomagnetic index Kp, both of them have a significant positive correlation with solar wind dynamic pressure; (2) H+ ion density is also observed to increase with solar wind dynamic pressure, and not correlated with geomagnetic index Kp. | GUO JianGuang SHI JianKui ZHANG TieLong LIU ZhenXing A. FAZAKERLEY H. REME I. DANDOURAS E. LUOEK | 2007 | Chinese Science Bulletin2007，52，7： | 3 |
| 5 | Continuous lobe reconnectionin the mid-tail and its relationship to substorms:Cluster observations of continuous lobe reconnection in the mid-magneto tail显示文摘When the IMF turns southward, a great amount of magnetic energy is stored in the magnetotail, and the electric field across the magnetotail substantially en-hances. As long as magnetic reconnection (MR) in the mag-netotail initiates and continues, the magnetic field and plasma in the central plasma sheet are carried away to the near-Earth and down to the tail, the magnetic field and plasma in the lobe region enter the CPS and are involved in MR. We call this process “Continuous Lobe Reconnection (CLR)”. In this paper a detailed analysis of Cluster observa-tion of MR through 2001―2003 is made. Plenty of CLR events are found that led to considerable changes of tail con-figuration, appearance of BBF, as well as large-scale bubbles in which both plasma temperature and number density sub-stantially decrease. It is shown that in general CLR events last for dozens of minutes and have good correspondence to substorm initiation under the condition of continuous southward IMF. | CAO Xin PU Zuyin ZHANG Hui FU Suiyan XIAO Chijie LIU Zhenxing J. B. cao A. Korth M. Frazen Q. G. Zong H. Reme K. H. Glassmeier | 2005 | Chinese Science Bulletin2005，50，18： | 2 |
| 6 | Analysis of the Interaction between Low-Frequency Waves and Ions in the High-Altitude Cusp Region Observed by Satellite Cluster显示文摘在离子(质子) 和在从 0.3 ~ 10 Hz 的频率范围 f (1 ) 的低频率波浪(LFW ) 之间的精力转移被穿过高高度的极的尖顶的簇观察。在低频率波浪和离子之间的精力转移有二个工具。一个人是精力从低频率被转移向离子和离子精力增加招手。其它是精力从离子被转移到低频率波浪和离子精力减少。离子旋转运动在精力转移过程起一个重要作用。LFW 能加速或速度的 f (1 ) 的电磁的地沿着周围的磁场的方向的质子并且温暖或使冷在周围的磁场的平行、垂直的方向的质子。质子数字密度的山峰价值有电磁的精力 oflow 频率波浪的相应山峰价值。这暗示运动 Alfven 波浪和独居的运动 Alfven 波浪可能在高高度的尖顶区域存在。 | 段素平 刘振兴 曹晋滨 史建魁 路立 李中元 Q. G. Zong H. Reme N. Cornilleau-Wehrlin A. Balogh M. Andre | 2006 | Chinese Physics Letters2006，23，5： | 2 |
| 7 | A Theoretic Interpretation of Movement of the Cusp Equatorward Boundary显示文摘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 Re to 9.0Re 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 C1 and C4 were crossing during same interval moved equatorward by 4.6°. The cusp equatorward boundary velocity computed in the theoretical model (10.7 km/s) is in good agreement with the observed value(9.4km/s) calculated from the data of CIS of Cluster C4 and C1. | J. B. Cao A. Leonovich G. C. Zhou Z. X. Liu H. Reme I. Dandouras | 2005 | 空间科学学报2005，25，5： | 2 |
| 8 | 磁层快速对流事件的多点卫星联合观测显示文摘本文利用星簇Cluster的三颗卫星(C1,C3和C4)在2001年和2002年的数据,研究了快速对流事件(RCE,Rapid Convection Event)及其与亚暴的关系.结果显示单点卫星对RCE的观测,不能反映磁尾RCE的真实情况.在2002年7月25日发生的一次RCE事件,C1和C3观测到这次RCE,C4却没有观测到.在三颗卫星联合观测到的306次RCE中,C1观测到215次,C3观测到266次,C4观测到227次.统计研究表明,单点卫星观测到的RCE的平均时间也不能准确反映磁层内的RCE.由此推论在整个中心等离子体片内,快速对流事件所承担的能量和磁通量的输运量,可能远大于单点卫星观测给出的结果.用速度来定义的磁尾爆发性整体流(BBF,Bursty Bulk Flow)与亚暴的关系,比用磁通量定义的RCE与亚暴的关系要更加紧密. | 马玉端 曹晋滨 周国成 刘振兴 H. Reme I. Dandouras E. Lucek | 2007 | 地球物理学报2007，50，5： | 1 |
| 9 | Multiple Flux Rope Events at the High-Latitude Magnetopause: Cluster/Rapid Observation on 26 January, 2001显示文摘 | Z. Y. Pu Q. -G. Zong T. A. Fritz C. J. Xiao Z. Y. Huang S. Y. Fu Q. Q. Shi M. W. Dunlop K. -H. Glassmeier A. Balogh P. Daly H. Reme J. Dandouras J. B. Cao Z. X. Liu C. Shen J. K. Shi | 2005 | Surveys in Geophysics (-)2005，，1： | 1 |
| 10 | Correlation between continuous lobe reconnection in the mid magnetotail and substorm expansion onset显示文摘Cluster/HIA 和 Cluster/FGM 在 2001 -2003 从 7 月在时期期间测量到 10 月的血浆表十字路口上的数据被分析。在连续脑叶的典型特征上基于以前的工作重新连接在参考,二案例研究和统计分析描述的离子(CLR ) 为发生在这个时期期间的事件在 midmagnetotail 和潜水艇暴风雨扩大发作在在 CLR 之间的关联上被执行。几乎所有 CLR 事件在有潜水艇暴风雨的靠近的连接,这被发现。CLR 的开始几乎总是是在在近的地球磁电机尾巴并且在基于 theground 的车站上看见的潜水艇暴风雨活动前的一些分钟。这提供 CLR 在连续向南方的星际间的磁场的时期期间是 substormexpansion 发作的虚拟原因的一个清楚的指示。 | ZHANG Hui PU Zuyin CAO Xin FU Suiyan XIAO Chijie LIU Zhenxing A. Korth M. Frazen ZONG Qiugong H. Reme K H Glassmeier R. Friedel G. D. Reeves M. W. Dunlop | 2006 | Chinese Science Bulletin2006，51，22： | 0 |
| 11 | 遗传性痴呆伴脑出血和脑血管淀粉样变 | Remes A.M. FinnilS. Mononen H. K.Majamaa 夏峰 | 2005 | 世界核心医学期刊文摘(神经病学分册)2005，0，1： | 0 |
| 12 | Structures of magnetic null points in reconnection diffusion region:Cluster observations显示文摘Magnetic reconnection is a very important and fundamental plasma process in transferring energy from magnetic field into plasma. Previous theory, numerical simulations and observations mostly concen-trate on 2-dimensional (2D) model; however, magnetic reconnection is a 3-dimensional (3D) nonlinear process in nature. The properties of reconnection in 3D and its associated singular structure have not been resolved completely. Here we investigate the structures and characteristics of null points inside the reconnection diffusion region by introducing the discretized Poincaré index through Gauss integral and using magnetic field data with high resolution from the four satellites of Cluster mission. We esti-mate the velocity and trajectory of null points by calculating its position in different times, and compare and discuss the observations with different reconnection models with null points based on character-istics of electric current around null points. | HU YunHui DENG XiaoHua ZHOU Meng TANG RongXin ZHAO Hui FU Song SU ZhiWen WANG JingFang YUAN ZhiGang R. NAKAMURA W. BAUMJOHANN H. REME C. M. CARR | 2008 | Chinese Science Bulletin2008，53，12： | 0 |
您所在的机构暂未开通此部分的功能，请联系管理员