Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections
Coronal mass ejections (CMEs) are the most energetic expulsions of magnetized plasma from the Sun that play a crucial role in space weather dynamics. This study investigates the diverse kinematics and thermodynamic evolution of two CMEs (CME1: 2011 September 24 and CME2: 2018 August 20) at coronal h...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad00ba |
| _version_ | 1797627525938020352 |
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| author | Soumyaranjan Khuntia Wageesh Mishra Sudheer K. Mishra Yuming Wang Jie Zhang Shaoyu Lyu |
| author_facet | Soumyaranjan Khuntia Wageesh Mishra Sudheer K. Mishra Yuming Wang Jie Zhang Shaoyu Lyu |
| author_sort | Soumyaranjan Khuntia |
| collection | DOAJ |
| description | Coronal mass ejections (CMEs) are the most energetic expulsions of magnetized plasma from the Sun that play a crucial role in space weather dynamics. This study investigates the diverse kinematics and thermodynamic evolution of two CMEs (CME1: 2011 September 24 and CME2: 2018 August 20) at coronal heights where thermodynamic measurements are limited. The peak 3D propagation speed of CME1 is high (1885 km s ^−1 ) with two-phase expansion (rapid and nearly constant), while the peak 3D propagation speed of CME2 is slow (420 km s ^−1 ) with only a gradual expansion. We estimate the distance-dependent variations in the polytropic index, heating rate, temperature, and internal forces implementing the revised FRIS model, taking inputs of 3D kinematics estimated from the graduated cylindrical shell model. We find CME1 exhibiting heat release during its early-rapid acceleration decrease and jumps to the heat-absorption state during its constant acceleration phase. In contrast to CME1, CME2 shows a gradual transition from the near-adiabatic to the heat-absorption state during its gradually increasing acceleration. Our analysis reveals that although both CMEs show differential heating, they experience heat absorption during their later propagation phases, approaching the isothermal state. The faster CME1 achieves an adiabatic state followed by an isothermal state at smaller distances from the Sun than the slower CME2. We also find that the expansion of CMEs is primarily influenced by centrifugal and thermal pressure forces, with the Lorentz force impeding expansion. Multiwavelength observations of flux-ropes at source regions support the FRIS-model-derived findings at initially observed lower coronal heights. |
| first_indexed | 2024-03-11T10:25:32Z |
| format | Article |
| id | doaj.art-38bfa9222163433e8cc5e3e6b388f522 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T10:25:32Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-38bfa9222163433e8cc5e3e6b388f5222023-11-15T13:31:12ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195819210.3847/1538-4357/ad00baUnraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass EjectionsSoumyaranjan Khuntia0https://orcid.org/0009-0006-3209-658XWageesh Mishra1https://orcid.org/0000-0003-2740-2280Sudheer K. Mishra2https://orcid.org/0000-0003-2129-5728Yuming Wang3https://orcid.org/0000-0002-8887-3919Jie Zhang4https://orcid.org/0000-0003-0951-2486Shaoyu Lyu5https://orcid.org/0000-0002-2349-7940Indian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; soumyaranjan.khuntia@iiap.res.in, wageesh.mishra@iiap.res.in; Pondicherry University , R.V. Nagar, Kalapet 605014, Puducherry, IndiaIndian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; soumyaranjan.khuntia@iiap.res.in, wageesh.mishra@iiap.res.inIndian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; soumyaranjan.khuntia@iiap.res.in, wageesh.mishra@iiap.res.in; Astronomical Observatory, Kyoto University , Sakyo, Kyoto 606-8502, JapanCAS Key Laboratory of Geospace Environment, Department of Geophysics and Planetary Sciences, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; ymwang@ustc.edu.cnDepartment of Physics and Astronomy, George Mason University , 4400 University Dr., MSN 3F3, Fairfax, VA 22030, USACAS Key Laboratory of Geospace Environment, Department of Geophysics and Planetary Sciences, University of Science and Technology of China , Hefei 230026, People’s Republic of China ; ymwang@ustc.edu.cnCoronal mass ejections (CMEs) are the most energetic expulsions of magnetized plasma from the Sun that play a crucial role in space weather dynamics. This study investigates the diverse kinematics and thermodynamic evolution of two CMEs (CME1: 2011 September 24 and CME2: 2018 August 20) at coronal heights where thermodynamic measurements are limited. The peak 3D propagation speed of CME1 is high (1885 km s ^−1 ) with two-phase expansion (rapid and nearly constant), while the peak 3D propagation speed of CME2 is slow (420 km s ^−1 ) with only a gradual expansion. We estimate the distance-dependent variations in the polytropic index, heating rate, temperature, and internal forces implementing the revised FRIS model, taking inputs of 3D kinematics estimated from the graduated cylindrical shell model. We find CME1 exhibiting heat release during its early-rapid acceleration decrease and jumps to the heat-absorption state during its constant acceleration phase. In contrast to CME1, CME2 shows a gradual transition from the near-adiabatic to the heat-absorption state during its gradually increasing acceleration. Our analysis reveals that although both CMEs show differential heating, they experience heat absorption during their later propagation phases, approaching the isothermal state. The faster CME1 achieves an adiabatic state followed by an isothermal state at smaller distances from the Sun than the slower CME2. We also find that the expansion of CMEs is primarily influenced by centrifugal and thermal pressure forces, with the Lorentz force impeding expansion. Multiwavelength observations of flux-ropes at source regions support the FRIS-model-derived findings at initially observed lower coronal heights.https://doi.org/10.3847/1538-4357/ad00baSolar coronal mass ejections |
| spellingShingle | Soumyaranjan Khuntia Wageesh Mishra Sudheer K. Mishra Yuming Wang Jie Zhang Shaoyu Lyu Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections The Astrophysical Journal Solar coronal mass ejections |
| title | Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections |
| title_full | Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections |
| title_fullStr | Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections |
| title_full_unstemmed | Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections |
| title_short | Unraveling the Thermodynamic Enigma between Fast and Slow Coronal Mass Ejections |
| title_sort | unraveling the thermodynamic enigma between fast and slow coronal mass ejections |
| topic | Solar coronal mass ejections |
| url | https://doi.org/10.3847/1538-4357/ad00ba |
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