SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy
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 more realistic results than traditional steady coronal models constrained by a static magnetogram. Howeve...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/add0b1 |
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| author | Haopeng Wang Liping Yang Stefaan Poedts Andrea Lani Yuhao Zhou Yuhang Gao Luis Linan Jiakun Lv Tinatin Baratashvili Jinhan Guo Rong Lin Zhan Su Caixia Li Man Zhang Wenwen Wei Yun Yang Yucong Li Xinyi Ma Edin Husidic Hyun-Jin Jeong Mahdi Najafi-Ziyazi Juan Wang Brigitte Schmieder |
| author_facet | Haopeng Wang Liping Yang Stefaan Poedts Andrea Lani Yuhao Zhou Yuhang Gao Luis Linan Jiakun Lv Tinatin Baratashvili Jinhan Guo Rong Lin Zhan Su Caixia Li Man Zhang Wenwen Wei Yun Yang Yucong Li Xinyi Ma Edin Husidic Hyun-Jin Jeong Mahdi Najafi-Ziyazi Juan Wang Brigitte Schmieder |
| author_sort | Haopeng Wang |
| collection | DOAJ |
| description | 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 more realistic results than traditional steady coronal models constrained by a static magnetogram. However, its practical application is significantly limited by the low computational efficiency and poor numerical stability in solving low- β issues common in coronal simulations. To address this, we propose an extended magnetic field decomposition strategy and successfully implement it in an implicit MHD coronal model. The traditional decomposition strategies split the magnetic field into a time-invariant potential field and a time-dependent component B _1 . This works well for quasi-steady-state coronal simulations where ∣ B _1 ∣ is typically small. However, when the inner-boundary magnetic field evolves, ∣ B _1 ∣ can grow significantly, and its discretization errors often lead to nonphysical negative thermal pressure, ultimately causing the simulation to crash. In the extended magnetic field decomposition strategy, we split the magnetic field into a temporally piecewise-constant field and a time-varying component, B _1 . This effectively keeps ∣ B _1 ∣ consistently small throughout the simulations and performs well in solving time-evolving low- β issues, thereby outperforming traditional methods. We incorporate this improved 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 observational features and performs more than 80 times faster than real-time evolutions using only 192 CPU cores, making it well suited for practical applications in simulating the time-evolving corona. |
| format | Article |
| id | doaj-art-c2caeca22ff044b29600bb40ce8233eb |
| institution | OA Journals |
| issn | 0067-0049 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj-art-c2caeca22ff044b29600bb40ce8233eb2025-08-20T02:08:57ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0127825910.3847/1538-4365/add0b1SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition StrategyHaopeng Wang0https://orcid.org/0000-0002-4217-6990Liping Yang1https://orcid.org/0000-0003-4716-2958Stefaan Poedts2https://orcid.org/0000-0002-1743-0651Andrea Lani3https://orcid.org/0000-0003-4017-215XYuhao Zhou4https://orcid.org/0000-0002-4391-393XYuhang Gao5https://orcid.org/0000-0002-6641-8034Luis Linan6https://orcid.org/0000-0002-4014-1815Jiakun Lv7Tinatin Baratashvili8https://orcid.org/0000-0002-1986-4496Jinhan Guo9https://orcid.org/0000-0002-4205-5566Rong Lin10https://orcid.org/0000-0001-7655-5000Zhan Su11Caixia Li12Man Zhang13https://orcid.org/0000-0003-3000-2819Wenwen Wei14https://orcid.org/0000-0001-8495-9179Yun Yang15https://orcid.org/0009-0000-5292-713XYucong Li16Xinyi Ma17Edin Husidic18https://orcid.org/0000-0002-1349-3663Hyun-Jin Jeong19https://orcid.org/0000-0003-4616-947XMahdi Najafi-Ziyazi20https://orcid.org/0009-0008-0922-3995Juan Wang21Brigitte Schmieder22https://orcid.org/0000-0003-3364-9183Centre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.beSIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of China ; lpyang@swl.ac.cnCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; Institute of Physics, University of Maria Curie-Skłodowska , ul. Radziszewskiego 10, 20-031 Lublin, PolandCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; Von Karman Institute for Fluid Dynamics , Waterloosesteenweg 72, 1640 Sint-Genesius-Rode, Brussels, BelgiumCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.beCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; School of Earth and Space Sciences, Peking University , Beijing 100871, People’s Republic of ChinaCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.beBeijing Institute of Applied Meteorology , Beijing 100029, People’s Republic of ChinaCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.beCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; School of Astronomy and Space Science and Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University , Nanjing 210023, People’s Republic of ChinaCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; School of Earth and Space Sciences, Peking University , Beijing 100871, People’s Republic of ChinaSIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of China ; lpyang@swl.ac.cn; College of Earth and Planetary Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaShenzhen Key Laboratory of Ultraintense Laser and Advanced Material Technology, Center for Intense Laser Application Technology, and College of Engineering Physics, Shenzhen Technology University , Shenzhen 518118, People’s Republic of ChinaSIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of China ; lpyang@swl.ac.cnSpace Sciences Laboratory, University of California , Berkeley, CA 94720, USASchool of Mathematical Sciences, Ministry of Education Key Laboratory for NSLSCS, Nanjing Normal University , Nanjing 210023, People’s Republic of ChinaCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; SIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of China ; lpyang@swl.ac.cn; College of Earth and Planetary Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaSIGMA Weather Group, State Key Laboratory of Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of China ; lpyang@swl.ac.cn; College of Earth and Planetary Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; Department of Physics and Astronomy, University of Turku , 20014 Turku, FinlandCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; School of Space Research, Kyung Hee University , Yongin, 17104, Republic of KoreaCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.beSchool of Systems Science, Beijing Normal University , Beijing 100875, People’s Republic of ChinaCentre for Mathematical Plasma-Astrophysics , Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium ; haopeng.wang1@kuleuven.be; Observatoire de Paris , LIRA, UMR8254 (CNRS), F-92195 Meudon Principal Cedex, France; SUPA, School of Physics & Astronomy, University of Glasgow , Glasgow G12 8QQ, UKTime-evolving magnetohydrodynamic (MHD) coronal modeling, driven by a series of time-dependent photospheric magnetograms, represents a new generation of coronal simulations. This approach offers more realistic results than traditional steady coronal models constrained by a static magnetogram. However, its practical application is significantly limited by the low computational efficiency and poor numerical stability in solving low- β issues common in coronal simulations. To address this, we propose an extended magnetic field decomposition strategy and successfully implement it in an implicit MHD coronal model. The traditional decomposition strategies split the magnetic field into a time-invariant potential field and a time-dependent component B _1 . This works well for quasi-steady-state coronal simulations where ∣ B _1 ∣ is typically small. However, when the inner-boundary magnetic field evolves, ∣ B _1 ∣ can grow significantly, and its discretization errors often lead to nonphysical negative thermal pressure, ultimately causing the simulation to crash. In the extended magnetic field decomposition strategy, we split the magnetic field into a temporally piecewise-constant field and a time-varying component, B _1 . This effectively keeps ∣ B _1 ∣ consistently small throughout the simulations and performs well in solving time-evolving low- β issues, thereby outperforming traditional methods. We incorporate this improved 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 observational features and performs more than 80 times faster than real-time evolutions using only 192 CPU cores, making it well suited for practical applications in simulating the time-evolving corona.https://doi.org/10.3847/1538-4365/add0b1The SunMagnetohydrodynamicsMagnetohydrodynamical simulationsSolar corona |
| spellingShingle | Haopeng Wang Liping Yang Stefaan Poedts Andrea Lani Yuhao Zhou Yuhang Gao Luis Linan Jiakun Lv Tinatin Baratashvili Jinhan Guo Rong Lin Zhan Su Caixia Li Man Zhang Wenwen Wei Yun Yang Yucong Li Xinyi Ma Edin Husidic Hyun-Jin Jeong Mahdi Najafi-Ziyazi Juan Wang Brigitte Schmieder SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy The Astrophysical Journal Supplement Series The Sun Magnetohydrodynamics Magnetohydrodynamical simulations Solar corona |
| title | SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy |
| title_full | SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy |
| title_fullStr | SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy |
| title_full_unstemmed | SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy |
| title_short | SIP-IFVM: A Time-evolving Coronal Model with an Extended Magnetic Field Decomposition Strategy |
| title_sort | sip ifvm a time evolving coronal model with an extended magnetic field decomposition strategy |
| topic | The Sun Magnetohydrodynamics Magnetohydrodynamical simulations Solar corona |
| url | https://doi.org/10.3847/1538-4365/add0b1 |
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