Simulation of turbulent magnetic reconnection in the smallscale solar wind

作     者：魏奉思 胡强 R.Schwen 冯学尚 

作者机构：Laboratory of Numerical Study for Heliospheric Physics Center for Space Science and Applied Research Chinese Academy of Sciences Beijing 100080 China Max-Planck-Institut fuer AeronomieD-37189 Katlenburg-LindauGermany 

出 版 物：《Science China Mathematics》 (中国科学：数学（英文版）)

年 卷 期：2000年第43卷第6期

页      面：629-637页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：the National Natural Science Foundation of China(49674243,49874040,49990450) the Knowledge Innovation Project, CAS 

主　　题：solar wind magnetic reconnection turbulence. 

摘      要：Some observational examples for the possible occurrence of the turbulent magnetic reconnection in the solar wind are found by analysing Helios spacecraft’s high resolution data. The phenomena of turbulent magnetic reconnections in small scale solar wind are simulated by introducing a third order accuracy upwind compact difference scheme to the compressible two-dimensional MHD flow. Numerical results verify that the turbulent magnetic reconnection process could occur in small scale interplanetary solar wind, which is a basic feature characterizing the magnetic reconnection in high-magnetic Replolds number (R(inM) = 2 000-10 000) solar wind. The configurations of the magnetic reconnection could evolve from a single X-line to a multiple X-line reconnection, exhibiting a complex picture of the formation, merging and evolution of magnetic islands, and finally the magnetic reconnection would evolve into a low-energy state. Its life-span of evolution is about one hour order of magnitude. Various magnetic and flow signatures are recorded in the numerical test for different evolution stages and along different crossing paths, which could in principle explain and confirm the observational samples from the Helios spacecraft. These results are helpful for revealing the basic physical processes in the solar wind turbulence.