2.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current Sheets
In the present paper, using MPI-AMRVAC , we perform a 2.5D numerical magnetohydrodynamic simulation of the dynamics and associated thermodynamical evolution of an initially force-free Harris current sheet subjected to an external velocity perturbation under the condition of uniform resistivity. The...
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad2079 |
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| author | Sripan Mondal Abhishek K. Srivastava David I. Pontin Ding Yuan Eric R. Priest |
| author_facet | Sripan Mondal Abhishek K. Srivastava David I. Pontin Ding Yuan Eric R. Priest |
| author_sort | Sripan Mondal |
| collection | DOAJ |
| description | In the present paper, using MPI-AMRVAC , we perform a 2.5D numerical magnetohydrodynamic simulation of the dynamics and associated thermodynamical evolution of an initially force-free Harris current sheet subjected to an external velocity perturbation under the condition of uniform resistivity. The amplitude of the magnetic field is taken to be 10 G, typical of the solar corona. We impose a Gaussian velocity pulse across this current sheet that mimics the interaction of fast magnetoacoustic waves with a current sheet in the corona. This leads to a variety of dynamics and plasma processes in the current sheet, which is initially quasi-static. The initial pulse interacts with the current sheet and splits into a pair of counterpropagating wavefronts, which form a rarefied region that leads to an inflow and a thinning of the current sheet. The thinning results in Petschek-type magnetic reconnection followed by a tearing instability and plasmoid formation. The reconnection outflows containing outward-moving plasmoids have accelerated motions with velocities ranging from 105 to 303 km s ^−1 . The average temperature and density of the plasmoids are found to be 8 MK and twice the background density of the solar corona, respectively. These estimates of the velocity, temperature, and density of the plasmoids are similar to values reported from various solar coronal observations. Therefore, we infer that the external triggering of a quasi-static current sheet by a single-velocity pulse is capable of initiating magnetic reconnection and plasmoid formation in the absence of a localized enhancement of resistivity in the solar corona. |
| first_indexed | 2024-04-25T02:14:52Z |
| format | Article |
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| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-25T02:14:52Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-553369416eb94409b0814ac7b36231eb2024-03-07T10:03:28ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01963213910.3847/1538-4357/ad20792.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current SheetsSripan Mondal0Abhishek K. Srivastava1David I. Pontin2Ding Yuan3Eric R. Priest4Department of Physics, Indian Institute of Technology (BHU) , Varanasi 221005, India ; asrivastava.app@iitbhu.ac.inDepartment of Physics, Indian Institute of Technology (BHU) , Varanasi 221005, India ; asrivastava.app@iitbhu.ac.inSchool of Information and Physical Sciences, University of Newcastle , AustraliaShenzhen Key Laboratory of Numerical Prediction for Space Storm , Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, Guangdong, People’s Republic of China ; yuanding@hit.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing, People’s Republic of ChinaMathematics Institute, St Andrews University , KY16 9SS, St Andrews, UKIn the present paper, using MPI-AMRVAC , we perform a 2.5D numerical magnetohydrodynamic simulation of the dynamics and associated thermodynamical evolution of an initially force-free Harris current sheet subjected to an external velocity perturbation under the condition of uniform resistivity. The amplitude of the magnetic field is taken to be 10 G, typical of the solar corona. We impose a Gaussian velocity pulse across this current sheet that mimics the interaction of fast magnetoacoustic waves with a current sheet in the corona. This leads to a variety of dynamics and plasma processes in the current sheet, which is initially quasi-static. The initial pulse interacts with the current sheet and splits into a pair of counterpropagating wavefronts, which form a rarefied region that leads to an inflow and a thinning of the current sheet. The thinning results in Petschek-type magnetic reconnection followed by a tearing instability and plasmoid formation. The reconnection outflows containing outward-moving plasmoids have accelerated motions with velocities ranging from 105 to 303 km s ^−1 . The average temperature and density of the plasmoids are found to be 8 MK and twice the background density of the solar corona, respectively. These estimates of the velocity, temperature, and density of the plasmoids are similar to values reported from various solar coronal observations. Therefore, we infer that the external triggering of a quasi-static current sheet by a single-velocity pulse is capable of initiating magnetic reconnection and plasmoid formation in the absence of a localized enhancement of resistivity in the solar corona.https://doi.org/10.3847/1538-4357/ad2079Solar atmosphereSolar coronaMagnetohydrodynamicsMagnetic fieldsSolar magnetic reconnection |
| spellingShingle | Sripan Mondal Abhishek K. Srivastava David I. Pontin Ding Yuan Eric R. Priest 2.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current Sheets The Astrophysical Journal Solar atmosphere Solar corona Magnetohydrodynamics Magnetic fields Solar magnetic reconnection |
| title | 2.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current Sheets |
| title_full | 2.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current Sheets |
| title_fullStr | 2.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current Sheets |
| title_full_unstemmed | 2.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current Sheets |
| title_short | 2.5D Magnetohydrodynamic Simulation of the Formation and Evolution of Plasmoids in Coronal Current Sheets |
| title_sort | 2 5d magnetohydrodynamic simulation of the formation and evolution of plasmoids in coronal current sheets |
| topic | Solar atmosphere Solar corona Magnetohydrodynamics Magnetic fields Solar magnetic reconnection |
| url | https://doi.org/10.3847/1538-4357/ad2079 |
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