Comparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence Simulations
This paper presents a comparison of plasma dynamics in coronal holes (CHs) and quiet Sun (QS) through 2.5D MHD flux emergence simulations. The magnetic reconnection between the emerging and the preexisting flux leads to the formation of cool, dense plasmoids with hot boundaries, and hot and cool jet...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/adc5fd |
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| author | Vishal Upendran Durgesh Tripathi Bhargav Vaidya Mark C. M. Cheung Takaaki Yokoyama |
| author_facet | Vishal Upendran Durgesh Tripathi Bhargav Vaidya Mark C. M. Cheung Takaaki Yokoyama |
| author_sort | Vishal Upendran |
| collection | DOAJ |
| description | This paper presents a comparison of plasma dynamics in coronal holes (CHs) and quiet Sun (QS) through 2.5D MHD flux emergence simulations. The magnetic reconnection between the emerging and the preexisting flux leads to the formation of cool, dense plasmoids with hot boundaries, and hot and cool jets with velocities ≈50 km s ^−1 . We perform a spectral synthesis in spectral lines probing transition region and coronal temperatures. CHs show reduced intensities, excess upflows (downflows), and widths during the jetting (downflow) period when compared to QS. During the jetting and downflow periods, the velocity and line width of the hot spectral lines in CHs show a strong positive correlation with the vertical magnetic field at z = 0, while the intensity of the cooler lines shows a weak correlation, which is not seen in QS. During the jetting period in CH, we find upflows in Si iv to be correlated (anticorrelated) with upflows (downflows) in other lines, and downflows in CH in Si iv to be correlated (anticorrelated) with upflows (downflows) in other lines when compared to QS. During the downflow, we find no strong correlation between Si iv and other line velocities. The correlation during the jetting period occurs due to coincident, cospatial origins of the hot and cool jet, while the lack of correlation during the downflow phase suggests a decoupling of hot and cool plasma. These results demonstrate that flux emergence and reconnection with preexisting flux in the atmosphere support a unified scenario for solar wind formation and coronal heating. |
| format | Article |
| id | doaj-art-49cbcc22a9af4be4bd4595a1dea74a4b |
| institution | OA Journals |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-49cbcc22a9af4be4bd4595a1dea74a4b2025-08-20T01:49:26ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198512710.3847/1538-4357/adc5fdComparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence SimulationsVishal Upendran0https://orcid.org/0000-0002-9253-6093Durgesh Tripathi1https://orcid.org/0000-0003-1689-6254Bhargav Vaidya2https://orcid.org/0000-0001-5424-0059Mark C. M. Cheung3https://orcid.org/0000-0003-2110-9753Takaaki Yokoyama4https://orcid.org/0000-0001-5457-4999SETI Institute , Mountain View, CA 94043, USA; Lockheed Martin Solar and Astrophysics Laboratory , Palo Alto, CA 94304, USA; Inter University Centre for Astronomy and Astrophysics , Pune, 411007, IndiaInter University Centre for Astronomy and Astrophysics , Pune, 411007, IndiaIndian Institute of Technology–Indore , Simrol, 452020, IndiaCSIRO , Space & Astronomy, Marsfield, NSW 2122, AustraliaAstronomical Observatory, Kyoto University , Kyoto, 606–8502, JapanThis paper presents a comparison of plasma dynamics in coronal holes (CHs) and quiet Sun (QS) through 2.5D MHD flux emergence simulations. The magnetic reconnection between the emerging and the preexisting flux leads to the formation of cool, dense plasmoids with hot boundaries, and hot and cool jets with velocities ≈50 km s ^−1 . We perform a spectral synthesis in spectral lines probing transition region and coronal temperatures. CHs show reduced intensities, excess upflows (downflows), and widths during the jetting (downflow) period when compared to QS. During the jetting and downflow periods, the velocity and line width of the hot spectral lines in CHs show a strong positive correlation with the vertical magnetic field at z = 0, while the intensity of the cooler lines shows a weak correlation, which is not seen in QS. During the jetting period in CH, we find upflows in Si iv to be correlated (anticorrelated) with upflows (downflows) in other lines, and downflows in CH in Si iv to be correlated (anticorrelated) with upflows (downflows) in other lines when compared to QS. During the downflow, we find no strong correlation between Si iv and other line velocities. The correlation during the jetting period occurs due to coincident, cospatial origins of the hot and cool jet, while the lack of correlation during the downflow phase suggests a decoupling of hot and cool plasma. These results demonstrate that flux emergence and reconnection with preexisting flux in the atmosphere support a unified scenario for solar wind formation and coronal heating.https://doi.org/10.3847/1538-4357/adc5fdSolar windSolar coronal heatingMagnetohydrodynamicsSolar magnetic flux emergenceSolar magnetic reconnectionSolar magnetic fields |
| spellingShingle | Vishal Upendran Durgesh Tripathi Bhargav Vaidya Mark C. M. Cheung Takaaki Yokoyama Comparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence Simulations The Astrophysical Journal Solar wind Solar coronal heating Magnetohydrodynamics Solar magnetic flux emergence Solar magnetic reconnection Solar magnetic fields |
| title | Comparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence Simulations |
| title_full | Comparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence Simulations |
| title_fullStr | Comparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence Simulations |
| title_full_unstemmed | Comparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence Simulations |
| title_short | Comparison of Plasma Dynamics in Coronal Holes and Quiet Sun Using Flux Emergence Simulations |
| title_sort | comparison of plasma dynamics in coronal holes and quiet sun using flux emergence simulations |
| topic | Solar wind Solar coronal heating Magnetohydrodynamics Solar magnetic flux emergence Solar magnetic reconnection Solar magnetic fields |
| url | https://doi.org/10.3847/1538-4357/adc5fd |
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