SIP-IFVM: A time-evolving coronal model with an extended magnetic field decomposition strategy
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arXiv
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| Format: | Preprint |
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2025
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| author | Wang, Haopeng Yang, Liping Poedts, Stefaan Lani, Andrea Zhou, Yuhao Gao, Yuhang Linan, Luis Lv, Jiakun Baratashvili, Tinatin Guo, Jinhan Lin, Rong Su, Zhan Li, Caixia Zhang, Man Wei, Wenwen Yang, Yun Li, Yucong Ma, Xinyi Husidic, Edin Jeong, Hyun-jin Mahdi, Najafi-Ziyazi Wang, Juan Schmieder, Brigitte |
| author_facet | Wang, Haopeng Yang, Liping Poedts, Stefaan Lani, Andrea Zhou, Yuhao Gao, Yuhang Linan, Luis Lv, Jiakun Baratashvili, Tinatin Guo, Jinhan Lin, Rong Su, Zhan Li, Caixia Zhang, Man Wei, Wenwen Yang, Yun Li, Yucong Ma, Xinyi Husidic, Edin Jeong, Hyun-jin Mahdi, Najafi-Ziyazi Wang, Juan Schmieder, Brigitte |
| contents | Time-evolving magnetohydrodynamic (MHD) coronal modeling, driven by a series of time-dependent photospheric magnetograms, represents a new generation of coronal simulations. This approach offers greater realism compared to traditional coronal models constrained by a static magnetogram. However, its practical application is seriously limited by low computational efficiency and poor numerical stability. Therefore, we propose an extended magnetic field decomposition strategy and implement it in the implicit MHD model to develop a coronal model that is both efficient and numerically stable enough for simulating the long-term evolutions of the global corona. The traditional decomposition strategies split the magnetic field into a time-invariant potential field and a time-dependent component $\mathbf{B}_1$. It works well for quasi-steady-state coronal simulations where $\left|\mathbf{B}_1\right|$ is typically small. However, as the inner-boundary magnetic field evolves, $\left|\mathbf{B}_1\right|$ can grow significantly larger and its discretization errors often lead to nonphysical negative thermal pressure, ultimately causing the code to crash. In this paper, we mitigate such undesired situations by introducing a temporally piecewise-constant variable to accommodate part of the non-potential field and remain $\left|\mathbf{B}_1\right|$ consistently small throughout the simulations. We incorporate this novel magnetic field decomposition strategy into our implicit MHD coronal model and apply it to simulate the evolution of coronal structures within 0.1 AU over two solar-maximum Carrington rotations. The results show that this coronal model effectively captures observations and performs more than 80 times faster than real time using only 192 CPU cores, making it well-suited for practical applications in simulating the time-evolving corona. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_07035 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | SIP-IFVM: A time-evolving coronal model with an extended magnetic field decomposition strategy Wang, Haopeng Yang, Liping Poedts, Stefaan Lani, Andrea Zhou, Yuhao Gao, Yuhang Linan, Luis Lv, Jiakun Baratashvili, Tinatin Guo, Jinhan Lin, Rong Su, Zhan Li, Caixia Zhang, Man Wei, Wenwen Yang, Yun Li, Yucong Ma, Xinyi Husidic, Edin Jeong, Hyun-jin Mahdi, Najafi-Ziyazi Wang, Juan Schmieder, Brigitte Solar and Stellar Astrophysics Time-evolving magnetohydrodynamic (MHD) coronal modeling, driven by a series of time-dependent photospheric magnetograms, represents a new generation of coronal simulations. This approach offers greater realism compared to traditional coronal models constrained by a static magnetogram. However, its practical application is seriously limited by low computational efficiency and poor numerical stability. Therefore, we propose an extended magnetic field decomposition strategy and implement it in the implicit MHD model to develop a coronal model that is both efficient and numerically stable enough for simulating the long-term evolutions of the global corona. The traditional decomposition strategies split the magnetic field into a time-invariant potential field and a time-dependent component $\mathbf{B}_1$. It works well for quasi-steady-state coronal simulations where $\left|\mathbf{B}_1\right|$ is typically small. However, as the inner-boundary magnetic field evolves, $\left|\mathbf{B}_1\right|$ can grow significantly larger and its discretization errors often lead to nonphysical negative thermal pressure, ultimately causing the code to crash. In this paper, we mitigate such undesired situations by introducing a temporally piecewise-constant variable to accommodate part of the non-potential field and remain $\left|\mathbf{B}_1\right|$ consistently small throughout the simulations. We incorporate this novel magnetic field decomposition strategy into our implicit MHD coronal model and apply it to simulate the evolution of coronal structures within 0.1 AU over two solar-maximum Carrington rotations. The results show that this coronal model effectively captures observations and performs more than 80 times faster than real time using only 192 CPU cores, making it well-suited for practical applications in simulating the time-evolving corona. |
| title | SIP-IFVM: A time-evolving coronal model with an extended magnetic field decomposition strategy |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2502.07035 |