Observational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration
Unstable states of the solar coronal magnetic field structure result in various flare behaviors. In this study, we compared the confined and eruptive flares that occurred under similar magnetic circumstances in the active region 12673, on 2017 September 6, using the twist number, decay index, and he...
Saved in:
| Main Authors: | , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/adc12d |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1850200541174431744 |
|---|---|
| author | Kouhei Teraoka Daiki Yamasaki Yusuke Kawabata Shinsuke Imada Toshifumi Shimizu |
| author_facet | Kouhei Teraoka Daiki Yamasaki Yusuke Kawabata Shinsuke Imada Toshifumi Shimizu |
| author_sort | Kouhei Teraoka |
| collection | DOAJ |
| description | Unstable states of the solar coronal magnetic field structure result in various flare behaviors. In this study, we compared the confined and eruptive flares that occurred under similar magnetic circumstances in the active region 12673, on 2017 September 6, using the twist number, decay index, and height of magnetic field lines to identify observational behaviors of the flare eruption. We investigated the parameters from the magnetic field lines involved in an initial energy release, which were identified from the positions of the core of flare ribbons, i.e., flare kernels. The magnetic field lines were derived by nonlinear force-free field modeling calculated from the photospheric vector magnetic field obtained by the Solar Dynamics Observatory SDO/Helioseismic and Magnetic Imager, and flare kernels were identified from the 1600 Å data obtained by the SDO/Atmospheric Imaging Assembly. The twist number of all the magnetic field lines in the confined flare was below 0.6; however, the twist number in seven out of 24 magnetic field lines in the eruptive flare was greater than 0.6. These lines were tall. It is found that the decay index is not a clear discriminator of the confined and eruptive flares. Our study suggests that some magnetic field lines in the kink instability state may be important for eruptive flares, and that taller magnetic field lines may promote flare eruption. |
| format | Article |
| id | doaj-art-10d2b25cefa94f9290e40b5c3d175c86 |
| 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-10d2b25cefa94f9290e40b5c3d175c862025-08-20T02:12:19ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01983212610.3847/1538-4357/adc12dObservational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic ConfigurationKouhei Teraoka0Daiki Yamasaki1https://orcid.org/0000-0003-1072-3942Yusuke Kawabata2https://orcid.org/0000-0001-7452-0656Shinsuke Imada3https://orcid.org/0000-0001-7891-3916Toshifumi Shimizu4https://orcid.org/0000-0003-4764-6856Department of Earth and Planetary Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan ; k-teraoka892@g.ecc.u-tokyo.ac.jp, shimizu.toshifumi@jaxa.jp; Institute of Space and Astronautical Science , Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, JapanInstitute of Space and Astronautical Science , Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanDepartment of Earth and Planetary Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan ; k-teraoka892@g.ecc.u-tokyo.ac.jp, shimizu.toshifumi@jaxa.jpDepartment of Earth and Planetary Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan ; k-teraoka892@g.ecc.u-tokyo.ac.jp, shimizu.toshifumi@jaxa.jp; Institute of Space and Astronautical Science , Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, JapanUnstable states of the solar coronal magnetic field structure result in various flare behaviors. In this study, we compared the confined and eruptive flares that occurred under similar magnetic circumstances in the active region 12673, on 2017 September 6, using the twist number, decay index, and height of magnetic field lines to identify observational behaviors of the flare eruption. We investigated the parameters from the magnetic field lines involved in an initial energy release, which were identified from the positions of the core of flare ribbons, i.e., flare kernels. The magnetic field lines were derived by nonlinear force-free field modeling calculated from the photospheric vector magnetic field obtained by the Solar Dynamics Observatory SDO/Helioseismic and Magnetic Imager, and flare kernels were identified from the 1600 Å data obtained by the SDO/Atmospheric Imaging Assembly. The twist number of all the magnetic field lines in the confined flare was below 0.6; however, the twist number in seven out of 24 magnetic field lines in the eruptive flare was greater than 0.6. These lines were tall. It is found that the decay index is not a clear discriminator of the confined and eruptive flares. Our study suggests that some magnetic field lines in the kink instability state may be important for eruptive flares, and that taller magnetic field lines may promote flare eruption.https://doi.org/10.3847/1538-4357/adc12dSolar flaresMagnetohydrodynamicsSolar magnetic reconnectionSolar physicsSolar coronal mass ejections |
| spellingShingle | Kouhei Teraoka Daiki Yamasaki Yusuke Kawabata Shinsuke Imada Toshifumi Shimizu Observational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration The Astrophysical Journal Solar flares Magnetohydrodynamics Solar magnetic reconnection Solar physics Solar coronal mass ejections |
| title | Observational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration |
| title_full | Observational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration |
| title_fullStr | Observational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration |
| title_full_unstemmed | Observational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration |
| title_short | Observational Comparison between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration |
| title_sort | observational comparison between confined and eruptive flares magnetohydrodynamics instability parameters in a similar magnetic configuration |
| topic | Solar flares Magnetohydrodynamics Solar magnetic reconnection Solar physics Solar coronal mass ejections |
| url | https://doi.org/10.3847/1538-4357/adc12d |
| work_keys_str_mv | AT kouheiteraoka observationalcomparisonbetweenconfinedanderuptiveflaresmagnetohydrodynamicsinstabilityparametersinasimilarmagneticconfiguration AT daikiyamasaki observationalcomparisonbetweenconfinedanderuptiveflaresmagnetohydrodynamicsinstabilityparametersinasimilarmagneticconfiguration AT yusukekawabata observationalcomparisonbetweenconfinedanderuptiveflaresmagnetohydrodynamicsinstabilityparametersinasimilarmagneticconfiguration AT shinsukeimada observationalcomparisonbetweenconfinedanderuptiveflaresmagnetohydrodynamicsinstabilityparametersinasimilarmagneticconfiguration AT toshifumishimizu observationalcomparisonbetweenconfinedanderuptiveflaresmagnetohydrodynamicsinstabilityparametersinasimilarmagneticconfiguration |