日冕三维太阳风模拟

刘畅; 沈芳; 刘佑生

doi:10.11728/cjss2022.01.201127102

日冕三维太阳风模拟

doi: 10.11728/cjss2022.01.201127102

中国科学院国家空间科学中心　北京　100190
中国科学院大学地球与行星科学学院　北京　100049

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

详细信息

作者简介:

刘畅　E-mail: cliu@spaceweather.ac.cn

通讯作者:

沈芳　沈芳，E-mail: fshen@spaceweather.ac.cn

中图分类号: P353
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出版历程
- 收稿日期: 2020-11-27
- 录用日期: 2021-04-12
- 修回日期: 2021-09-07
- 网络出版日期: 2022-05-25

Three-dimensional Numerical Simulation of Coronal Solar Wind

National Space Science Center, Chinese Academy of Sciences, Beijing 100190
College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing 100049

摘要

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。
- COIN-TVD MHD模型 /
- 磁场散度误差 /
- 磁流体模拟 /
- 日冕加热加速
Abstract: 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.
- COIN-TVD MHD model /
- Magnetic field divergence error /
- Magnetohydrodynamic numerical simulation /
- Coronal heating and acceleration

HTML全文

图 1 CR2199 GONG的全球磁场

Figure 1. CR2199 global magnetic field overview from GONG

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图 2 模拟得到的模型A和模型B从1R_s到22.5 R_s的位于子午面上的磁场及径向速度。流线表示磁力线，等值线表示径向速度

Figure 2. Results of the magnetic field lines and radial speed obtained by Model A and Model B from 1 R_s to 22.5 R_s. The streamline represents the magnetic line of force, and the equivalent line represents the radial speed

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图 3 模拟得到的模型A和模型B从1 R_s到22.5 R_s的位于子午面上的磁场及温度。流线表示磁力线，等值线表示温度

Figure 3. Results of the magnetic field lines and temperature obtained by Model A and Model B from 1 R_s to 22.5 R_s. The streamline represents the magnetic line of force and the equivalent line represents the temperature

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图 4 模拟得到的模型A和模型B从1 R_s到22.5 R_s的位于子午面上的磁场及密度。流线表示磁力线，等值线表示密度

Figure 4. Results of the magnetic field lines and numerical density obtained by Model A and Model B from 1 R_s to 22.5 R_s. The streamline represents the magnetic line of force and the equivalent line represents the number density

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图 5 使用扩散法模拟得到的从1 R_s到22.5 R_s的磁场相对散度误差位于子午面 $ \phi $=180°－0° (a)和$ \phi $=270°－90° (b) 上的分布

Figure 5. Relative Error of magnetic field divergence obtained by diffusive method on the meridional plane of $ \phi $=180°－0°(a) and $ \phi $=270°－90°(b) from 1 R_s to 22.5 R_s

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图 6 使用八波法模拟得到的从1 R_s到22.5 R_s的磁场相对散度误差位于子午面 $ \phi $=180°－0° (a)和$ \phi $=270°－90° (b)上的分布

Figure 6. Relative error of magnetic field divergence obtained by Powell method on the meridional plane of $ \phi $=180°－0°(a) and $ \phi $=270°－90°(b) from 1 R_s to 22.5 R_s

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图 7 使用扩散八波法模拟得到的从1 R_s到22.5 R_s的磁场相对散度误差位于子午面$ \phi $=180°－0° (a)和$ \phi $=270°－90° (b)上的分布

Figure 7. Relative error of magnetic field divergence obtained by Diffusive and Powell method on the meridional plane of $ \phi $=180°－0°(a) and $ \phi $=270°－90°(b) from 1 R_s to 22.5 R_s

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