Three Dimensional Simulation of the Steady Solar Wind in Carrington Rotation 1935  

作　　者：XIANG Changqing FENG Xueshang YAO Jiusheng 

机构地区：[1]Key Laboratory for Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100080

出　　处：《空间科学学报》2006年第1期8-13,共6页Chinese Journal of Space Science

基　　金：Supported by the National Natural Science Foundation of China (40374056, 40204010, 40536029)the International Collaboration Research Team Program of the Chinese Academy of Sciences

摘　　要：A three-dimensional MHD simulation is conducted to study the steady solar wind in Carrington Rotation (CR) 1935 by using the three-dimensional numerical magnetohydrodynamic (MHD) model introduced by Feng et al The numerical results demonstrate that the neutral current sheet has two peaks and two valleys, which is consistent with the result of PFSS model at Wilcox Solar Observatory (WSO). The obtained proton number density at 2.5 Rs is of the same order of magnitude as the result estimated from K-coronal brightness during the CRs 1733-1742 in 1983 made by Wei et al. The radial velocity profile along heliocentric distance is consistent with that of low solar wind speed deduced by Sheeley and Wang et al. However, it is not able to reproduce the fast-speed flow in coronal holes and slow solar wind in streamers because of oversimplified energy equation adopted in our model. Future efforts must be made to remedy this deficiency.A three-dimensional MHD simulation is conducted to study the steady solar wind in Carrington Rotation （CR） 1935 by using the three-dimensional numerical magnetohydrodynamic （MHD） model introduced by Feng et al. The numerical results demonstrate that the neutral current sheet has two peaks and two valleys, which is consistent with the result of PFSS model at Wilcox Solar Observatory （WSO）. The obtained proton number density at 2.5 Rs is of the same order of magnitude as the result estimated from K-coronal brightness during the CRs 1733-1742 in 1983 made by Wei et al. The radial velocity profile along heliocentric distance is consistent with that of low solar wind speed deduced by Sheeley and Wang et al. However, it is not able to reproduce the fast-speed flow in coronal holes and slow solar wind in streamers because of oversimplified energy equation adopted in our model. Future efforts must be made to remedy this deficiency.

关 键 词：三维模拟 太阳风 空间物理 地球物理 

分 类 号：P35[天文地球—空间物理学]