NSSC OpenIR  > 空间科学部
1998年5月日冕三维结构的数值模拟
Alternative TitleTHREE-DIMENSIONAL NUMERICAL CORONAL MODEL OF CARRINGTON ROTATION 1935 AT MAY 1998
叶占银; 魏奉思; 冯学尚; 石勇; 姚久胜; 北京8701信箱
Department空间天气学国家重点实验室
Source Publication空间科学学报
2001
Volume21Issue:4Pages:289-296
ISSN0254-6124
Language中文
Keyword三维理想磁流体力模式 Mhd数值模拟 日冕三维结构 日地空间太阳风
Abstract采用三维理想磙流体力学(MHD)模式,内边界条件把二维投影特征线边界方法推广应用到三维计算,有效地稳定了数值计算并保证稳态解的自洽性;初始猜解磁场由1935卡林顿周光球磁场观测数据得到,这样计算得到的1998年5月份期间日冕三维结构比较符合实际,计算结果表明:(1)计算得到的源表面非径向磁场量值在磁中性线附近不超过2μT,表明源表面磁场基本径向.(2)模拟得到的源表面径向磁场量值除了在磁中性线附近的区域外变化不大,这和观测一致.(3)由源表面磁场按平方反比的规律计算出1AU处磁场量值更接近观测值.(4)计算得到的日冕结构和观测定性一致,三维数值模拟结果表明,日冕的三维大尺度背景结构主要是由磁场决定的,在闭磁场处或者电流片附近,太阳风的密度高,速度低;在开场区,太阳风的密度低,速度高.
Other AbstractThree-dimensional coronal structure of Carrington rotation 1935 at May 1998 is obtained by using a three-dimensional numerical model of ideal magnetohydro-dynamic equations.In this numerical model,MacCormark-II scheme is employed for the discretization of the governing equations in computational domain and non-reflecting projected-characteristic condition is adopted at inner boundary to keep the simulation stable and the solution self-consistent.With the numerical model,iteration is carried out with initial magnetic field constructed from photosphere observation at 1935 Carrington rotation by Legendre series expansion and finally approaches a steady state.The iteration results show that:(1) magnetic field on source surface is nearly in radial direction with non-radial magnetic field compo-nent no more than 2 Tnear the neutral line.(2)The value of radial magnetic field component on source surface has no much variation except near the neutral line.This agrees with Ulysess observation.(3) The magnitude of radial magnetic field component at 1 AU, calculated from that on source surface by rule of r-2, approxi-mates observation better than that obtained by potential model.(4) 3-D numerical coronal structure agrees qualitatively with observation.The 3-D numerical results also show that magnetic field dominates global solar wind structure,in which den-sity of solar wind is high and speed is low in close magnetic field and near current sheet, while density is low and speed is high at open magnetic field.
Indexed ByCSCD
Funding Project中国科学院空间科学与应用研究中心
Citation statistics
Document Type期刊论文
Version出版稿
Identifierhttp://ir.nssc.ac.cn/handle/122/1295
Collection空间科学部
Corresponding Author北京8701信箱
Recommended Citation
GB/T 7714
叶占银,魏奉思,冯学尚,等. 1998年5月日冕三维结构的数值模拟[J]. 空间科学学报,2001,21(4):289-296.
APA 叶占银,魏奉思,冯学尚,石勇,姚久胜,&北京8701信箱.(2001).1998年5月日冕三维结构的数值模拟.空间科学学报,21(4),289-296.
MLA 叶占银,et al."1998年5月日冕三维结构的数值模拟".空间科学学报 21.4(2001):289-296.
Files in This Item:
File Name/Size DocType Version Access License
2001214289.pdf(704KB) 开放获取CC BY-NC-SAApplication Full Text
Related Services
Recommend this item
Bookmark
Usage statistics
Export to Endnote
Google Scholar
Similar articles in Google Scholar
[叶占银]'s Articles
[魏奉思]'s Articles
[冯学尚]'s Articles
Baidu academic
Similar articles in Baidu academic
[叶占银]'s Articles
[魏奉思]'s Articles
[冯学尚]'s Articles
Bing Scholar
Similar articles in Bing Scholar
[叶占银]'s Articles
[魏奉思]'s Articles
[冯学尚]'s Articles
Terms of Use
No data!
Social Bookmark/Share
All comments (0)
No comment.
 

Items in the repository are protected by copyright, with all rights reserved, unless otherwise indicated.