日冕三维太阳风模拟  

Three-dimensional Numerical Simulation of Coronal Solar Wind

作　　者：刘畅 沈芳 刘佑生 LIU Chang;SHEN Fang;LIU Yousheng(National Space Science Center,Chinese Academy of Sciences,Beijing 100190;College of Earth and Planetary Sciences,University of Chinese Academy of Sciences,Beijing 100049)

机构地区：[1]中国科学院国家空间科学中心,北京100190 [2]中国科学院大学地球与行星科学学院,北京100049

出　　处：《空间科学学报》2022年第1期25-33,共9页Chinese Journal of Space Science

基　　金：国家自然科学基金项目(41774184,41974202);国家重点实验室专项研究基金项目共同资助。

摘　　要：COIN-TVD MHD模型是近年发展起来的能有效实现日冕–行星际三维太阳风模拟的模型。本文利用此模型针对日冕区三维太阳风进行研究,为了模拟日冕太阳风的加热加速,对模型中的体积加热项做了调整。在磁流体模拟中,减小磁场散度的误差是关键问题之一,在调整体积加热项后应用扩散法、八波法、扩散八波法,对2199卡林顿周的背景太阳风进行模拟。模拟结果符合日冕太阳风结构,而且扩散八波法处理磁场散度性能有提升,可将相对磁场散度误差可控制在10^(-9)量级上。The Coronal Interplanetary-Total Variation Diminishing(COIN-TVD) magnetohydrodynamic(MHD) model developed in recent years that can effectively realize the coronal-interplanetary three-dimensional(3D) solar wind simulation. In this paper, the 3D coronal solar wind is studied by using this model. In order to simulate the heating and acceleration of solar wind in coronal region, the volume heating term in the model is improved. For MHD simulations, one of the key problems is to remove the magnetic field divergence error. Then, the influence of different methods to reduce the magnetic field divergence error on the coronal solar wind structure is discussed. The background solar wind of CR2199 is simulated by the diffusive method, Powell method, Diffusive and Powell method. The simulation results are consistent with the features of the coronal solar wind. The Diffusive and Powell method can control the relative magnetic field divergence error at the order of 10^(-9).

关 键 词：COIN-TVD MHD模型 磁场散度误差 磁流体模拟 日冕加热加速 

分 类 号：P353[天文地球—空间物理学]