Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection
Coronal mass ejections are explosive plasma phenomena prevalently occurring on the Sun and probably on other magnetically active stars. However, how their pre-eruptive configuration evolves toward the main explosion remains elusive. Here, based on comprehensive observations of a long-duration precur...
| 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 Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/acf3e4 |
| _version_ | 1797683723923095552 |
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| author | X. Cheng C. Xing G. Aulanier S. K. Solanki H. Peter M. D. Ding |
| author_facet | X. Cheng C. Xing G. Aulanier S. K. Solanki H. Peter M. D. Ding |
| author_sort | X. Cheng |
| collection | DOAJ |
| description | Coronal mass ejections are explosive plasma phenomena prevalently occurring on the Sun and probably on other magnetically active stars. However, how their pre-eruptive configuration evolves toward the main explosion remains elusive. Here, based on comprehensive observations of a long-duration precursor in an event on 2012 March 13, we determine that the heating and slow rise of the pre-eruptive hot magnetic flux rope (MFR) are achieved through a precursor reconnection located above cusp-shaped high-temperature precursor loops. It is observed that the hot MFR threads are built up continually, with their middle initially showing an “M” shape and then being separated from the cusp of precursor loops, causing the slow rise of the entire MFR. The slow rise, in combination with the thermal-dominated hard X-ray source concentrated at the top of the precursor loops, shows that the precursor reconnection is much weaker than the flare reconnection of the main eruption. We also perform a 3D magnetohydrodynamics simulation that reproduces the early evolution of the MFR transiting from the slow to fast rise. It is revealed that the magnetic tension force pertinent to “M”-shaped threads drives the slow rise, which, however, evolves into a magnetic pressure gradient-dominated regime responsible for the rapid acceleration eruption. |
| first_indexed | 2024-03-12T00:19:55Z |
| format | Article |
| id | doaj.art-1c59e0b627a543f68c7539f4a73882cf |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-12T00:19:55Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj.art-1c59e0b627a543f68c7539f4a73882cf2023-09-15T13:55:41ZengIOP PublishingThe Astrophysical Journal Letters2041-82052023-01-019542L4710.3847/2041-8213/acf3e4Deciphering the Slow-rise Precursor of a Major Coronal Mass EjectionX. Cheng0https://orcid.org/0000-0003-2837-7136C. Xing1https://orcid.org/0000-0002-6550-1522G. Aulanier2S. K. Solanki3https://orcid.org/0000-0002-3418-8449H. Peter4https://orcid.org/0000-0001-9921-0937M. D. Ding5https://orcid.org/0000-0002-4978-4972School of Astronomy and Space Science, Nanjing University , Nanjing 210093, People’s Republic of China ; xincheng@nju.edu.cn; Max Planck Institute for Solar System Research , Göttingen D-37077, GermanySchool of Astronomy and Space Science, Nanjing University , Nanjing 210093, People’s Republic of China ; xincheng@nju.edu.cn; Sorbonne Université, Observatoire de Paris—PSL, École Polytechnique, Institut Polytechnique de Paris , CNRS, Laboratoire de physique des plasmas (LPP), 4 place Jussieu, F-75005 Paris, FranceSorbonne Université, Observatoire de Paris—PSL, École Polytechnique, Institut Polytechnique de Paris , CNRS, Laboratoire de physique des plasmas (LPP), 4 place Jussieu, F-75005 Paris, France; Rosseland Centre for Solar Physics, Institute for Theoretical Astrophysics , Universitetet i Oslo, P.O. Box 1029, Blindern, NO-0315 Oslo, NorwayMax Planck Institute for Solar System Research , Göttingen D-37077, GermanyMax Planck Institute for Solar System Research , Göttingen D-37077, GermanySchool of Astronomy and Space Science, Nanjing University , Nanjing 210093, People’s Republic of China ; xincheng@nju.edu.cnCoronal mass ejections are explosive plasma phenomena prevalently occurring on the Sun and probably on other magnetically active stars. However, how their pre-eruptive configuration evolves toward the main explosion remains elusive. Here, based on comprehensive observations of a long-duration precursor in an event on 2012 March 13, we determine that the heating and slow rise of the pre-eruptive hot magnetic flux rope (MFR) are achieved through a precursor reconnection located above cusp-shaped high-temperature precursor loops. It is observed that the hot MFR threads are built up continually, with their middle initially showing an “M” shape and then being separated from the cusp of precursor loops, causing the slow rise of the entire MFR. The slow rise, in combination with the thermal-dominated hard X-ray source concentrated at the top of the precursor loops, shows that the precursor reconnection is much weaker than the flare reconnection of the main eruption. We also perform a 3D magnetohydrodynamics simulation that reproduces the early evolution of the MFR transiting from the slow to fast rise. It is revealed that the magnetic tension force pertinent to “M”-shaped threads drives the slow rise, which, however, evolves into a magnetic pressure gradient-dominated regime responsible for the rapid acceleration eruption.https://doi.org/10.3847/2041-8213/acf3e4Solar coronal mass ejectionsSolar magnetic reconnectionSolar flaresMagnetohydrodynamics |
| spellingShingle | X. Cheng C. Xing G. Aulanier S. K. Solanki H. Peter M. D. Ding Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection The Astrophysical Journal Letters Solar coronal mass ejections Solar magnetic reconnection Solar flares Magnetohydrodynamics |
| title | Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection |
| title_full | Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection |
| title_fullStr | Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection |
| title_full_unstemmed | Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection |
| title_short | Deciphering the Slow-rise Precursor of a Major Coronal Mass Ejection |
| title_sort | deciphering the slow rise precursor of a major coronal mass ejection |
| topic | Solar coronal mass ejections Solar magnetic reconnection Solar flares Magnetohydrodynamics |
| url | https://doi.org/10.3847/2041-8213/acf3e4 |
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