杨子才^1,2,3,,
沈芳^1,2,3,4,,,
杨易^1,3,
冯学尚^1,3,4
1. 中国科学院国家空间科学中心空间天气学国家重点实验室, 北京 100190
2. 山东省光学天文与日地空间环境重点实验室, 山东大学(威海), 山东威海 264209
3. 中国科学院大学, 北京 100049
4. 哈尔滨工业大学(深圳)空间科学与应用技术研究院, 深圳 518055

基金项目: 国家自然科学基金（41474152，41531073，41774184）、空间天气学国家重点实验室专项研究基金、山东省光学天文与日地空间环境重点实验室专项基金和国家"****"青年拔尖人才项目共同资助


详细信息

作者简介: 杨子才, 男, 主要从事日地空间背景太阳风结构的三维MHD数值模拟.E-mail:zcyang@spaceweather.ac.cn

通讯作者: 沈芳, 女, 主要从事日地空间背景太阳风结构以及行星际扰动传播过程的三维MHD数值模拟.E-mail:fshen@spaceweather.ac.cn

中图分类号: P353

收稿日期:2018-01-08
修回日期:2018-09-30
上线日期:2018-11-05

Three-dimensional MHD simulation of interplanetary solar wind

YANG ZiCai^1,2,3,,
SHEN Fang^1,2,3,4,,,
YANG Yi^1,3,
FENG XueShang^1,3,4
1. State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
2. Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Shandong University(Weihai), Shandong Weihai 264209, China
3. University of Chinese Academy of Sciences, Beijing 100049, China
4. HIT Institute of Space Science and Applied Technology, Shenzhen 518055, China


More Information

Corresponding author: SHEN Fang,E-mail:fshen@spaceweather.ac.cn

MSC: P353

--> Received Date: 08 January 2018
Revised Date: 30 September 2018
Available Online: 05 November 2018


摘要
摘要:近地空间的太阳风参数预报具有重要的科学研究意义和实际应用价值，三维磁流体力学（MHD）数值模拟是太阳风参数预报的重要手段.本文建立了一套基于经验模型的三维MHD数值模型.模型的内边界设置在0.1天文单位（AU）处，在六片网格系统下利用TVD Lax-Friedrich格式求解理想MHD方程组，采用扩散法消除磁场的散度.模型以GONG的观测磁图作为输入数据，利用经验模型并结合卫星观测特征确定内边界条件.边界条件中保留了6个可调参数，以便适当调整参数使其方便适合模拟不同太阳活动期的太阳风.利用该模型分别模拟了2007年和2016年的背景太阳风，得到了太阳风速度、密度、温度和磁场强度，这些参数与ACE/WIND卫星观测符合较好.
关键词: MHD/
太阳风/
模拟/
预报

Abstract:The prediction of solar wind parameters near the Earth has important scientific research significance and practical application value. Three-dimensional magnetohydrodynamics (MHD) numerical simulation is a primary tool in the prediction of solar wind parameters. This paper presents a three-dimensional MHD numerical model which can be used to simulate the background solar wind in the interplanetary space. The inner boundary of the model is set at 0.1 astronomical unit (AU) and a six-component grid system is employed in the computation domain. The ideal MHD equations are solved by using the total variation diminution (TVD) Lax-Friedrich scheme, and the divergence of the magnetic field is eliminated by a diffusion method. This model uses magnetogram synoptic map images from the Global Oscillation Network Group (GONG) observation as input data. The empirical Wang-Sheeley-Arge (WSA) relation is used to assign solar wind speed at the inner boundary, while density and temperature are specified according to the characteristics of satellite observations. There are six free parameters in the boundary conditions, which can be tuned to simulate the solar wind for different phases of the solar cycle. This model is used to simulate the background solar wind in 2007 and 2016, respectively, and the simulated solar wind parameters (including speed, density, temperature, and the magnetic field strength) are in good agreement with the ACE/WIND satellite observations.
Key words:MHD/
Solar wind/
Simulation/
Prediction



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