Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Fast-mode magnetohydrodynamic waves in the solar corona are often known to be produced by solar flares and eruptive prominences. Here, we simulate the effect of the interaction of an external perturbation on a magnetic null in the solar corona, which results in the formation of a current sheet (CS)....
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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/ad9022 |
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| author | Sripan Mondal Abhishekh Kumar Srivastava David I. Pontin Eric R. Priest R. Y. Kwon Ding Yuan |
| author_facet | Sripan Mondal Abhishekh Kumar Srivastava David I. Pontin Eric R. Priest R. Y. Kwon Ding Yuan |
| author_sort | Sripan Mondal |
| collection | DOAJ |
| description | Fast-mode magnetohydrodynamic waves in the solar corona are often known to be produced by solar flares and eruptive prominences. Here, we simulate the effect of the interaction of an external perturbation on a magnetic null in the solar corona, which results in the formation of a current sheet (CS). Once the CS undergoes a sufficient extension in its length and squeezing of its width, it may become unstable to the formation of multiple impulsive plasmoids. Eventually, the plasmoids merge with one another to form larger plasmoids and/or are expelled from the sheet. The formation, motion, and coalescence of plasmoids with each other and with magnetic Y-points at the outer periphery of the extended CS are found to generate wavelike perturbations. An analysis of the resultant quasiperiodic variations of pressure, density, velocity, and magnetic field at certain locations in the model corona indicates that these waves are predominantly fast-mode magnetoacoustic waves. For typical coronal parameters, the resultant propagating waves carry an energy flux of 10 ^5 erg cm ^−2 s ^−1 to a large distance of at least 60 Mm away from the CS. In general, we suggest that both waves and reconnection play a role in heating the solar atmosphere and driving the solar wind and may interact with one another in a manner that we refer to as a “symbiosis of waves and reconnection.” |
| format | Article |
| id | doaj-art-3665f20ca1b7405d91c160f7b91ff71d |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| spelling | doaj-art-3665f20ca1b7405d91c160f7b91ff71d2024-12-17T07:45:45ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01977223510.3847/1538-4357/ad9022Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty ReconnectionSripan Mondal0Abhishekh Kumar Srivastava1https://orcid.org/0000-0002-1641-1539David I. Pontin2Eric R. Priest3R. Y. Kwon4Ding Yuan5https://orcid.org/0000-0002-9514-6402Department 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 , Callaghan, NSW 2308, AustraliaMathematics Institute, St Andrews University , KY16 9SS, St Andrews, UKKorea Astronomy and Space Science Institute , Daejeon 34055, Republic of KoreaShenzhen 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.cnFast-mode magnetohydrodynamic waves in the solar corona are often known to be produced by solar flares and eruptive prominences. Here, we simulate the effect of the interaction of an external perturbation on a magnetic null in the solar corona, which results in the formation of a current sheet (CS). Once the CS undergoes a sufficient extension in its length and squeezing of its width, it may become unstable to the formation of multiple impulsive plasmoids. Eventually, the plasmoids merge with one another to form larger plasmoids and/or are expelled from the sheet. The formation, motion, and coalescence of plasmoids with each other and with magnetic Y-points at the outer periphery of the extended CS are found to generate wavelike perturbations. An analysis of the resultant quasiperiodic variations of pressure, density, velocity, and magnetic field at certain locations in the model corona indicates that these waves are predominantly fast-mode magnetoacoustic waves. For typical coronal parameters, the resultant propagating waves carry an energy flux of 10 ^5 erg cm ^−2 s ^−1 to a large distance of at least 60 Mm away from the CS. In general, we suggest that both waves and reconnection play a role in heating the solar atmosphere and driving the solar wind and may interact with one another in a manner that we refer to as a “symbiosis of waves and reconnection.”https://doi.org/10.3847/1538-4357/ad9022Active solar corona |
| spellingShingle | Sripan Mondal Abhishekh Kumar Srivastava David I. Pontin Eric R. Priest R. Y. Kwon Ding Yuan Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection The Astrophysical Journal Active solar corona |
| title | Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection |
| title_full | Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection |
| title_fullStr | Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection |
| title_full_unstemmed | Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection |
| title_short | Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection |
| title_sort | generation of fast magnetoacoustic waves in the corona by impulsive bursty reconnection |
| topic | Active solar corona |
| url | https://doi.org/10.3847/1538-4357/ad9022 |
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