| 基于MHD模拟数据的正午午夜子午面磁层顶位形研究 |
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| 引用本文： | 刘慧莲,黄朝晖.基于MHD模拟数据的正午午夜子午面磁层顶位形研究[J].空间科学学报,2011,31(1). |
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| 作者姓名： | 刘慧莲 黄朝晖 |
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| 作者单位： | 1. 中国科学院空间科学与应用研究中心,空间天气学国家重点实验室,北京,100190;中国科学院研究生院,北京,100049
2. 中国科学院空间科学与应用研究中心,空间天气学国家重点实验室,北京,100190 |
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| 基金项目： | 国家自然科学基金项目(40974106,40674082,40921063,40831060); 中国科学院“十一五”信息化专项(INFO-115-D01-Z0011)共同资助 |
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| 摘 要： | 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D_p与行星际磁场分量B_z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r_0增大;行星际磁场为南向时,磁场增强,磁层顶日下点距离r_0减小.整体而言,行星际磁场分量B_z由南转北时,r_0增大,且B_z对r_0的影响减弱.太阳风动压D_p是控制磁层顶日下点的主要因素,D_p增大,r_0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;D_p增大,α略增大,这意味着D_p对磁通量由日侧向夜侧的传输也有一定的贡献.
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| 关 键 词： | 日下点距离 磁层顶张角 磁层顶电流密度 |
Size and Shape of Magnetopause in the Noon-midnight Meridian Plane Based on the MHD Simulation |
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| LIU Huilian,HUANG Zhaohui.Size and Shape of Magnetopause in the Noon-midnight Meridian Plane Based on the MHD Simulation[J].Chinese Journal of Space Science,2011,31(1). |
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| Authors: | LIU Huilian HUANG Zhaohui |
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| Institution: | LIU Huilian~(1,2) HUANG Zhaohui~1 1(State Key Laboratory of Space Weather,Center for Space Science and Applied Research,Chinese Academy of Sciences,Beijing 100190) 2(Graduate University of Chinese Academy of Sciences,Beijing 100049) |
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| Abstract: | A quantitative model about the location and Shape of Magnetopause(MP) in the noon-midnight meridian plane is given by analyzing the computing data from three-dimensional global MHD simulation of the magnetosphere.Data processing results show the function which was presented by Ref.3]based on the satellite observational data can also be used to describe MP in noon-midnight meridian plane.The location and shape of the MP in the noon-midnight meridian plane are more complicated than those in the equatorial pl... |
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| Keywords: | Standoff distance Level of the tail flaring Magnetopause current density |
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