Evolution of coronal magnetic field parameters during X5.4 solar flare
The coronal magnetic field over NOAA Active Region 11,429 during a X5.4 solar flare on 7 March 2012 is modeled using optimization based Non-Linear Force-Free Field extrapolation. Specifically, 3D magnetic fields were modeled for 11 timesteps using the 12-min cadence Solar Dynamics Observatory (SDO)...
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| Format: | Article |
| Language: | English |
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Frontiers Media S.A.
2023-03-01
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| Series: | Frontiers in Astronomy and Space Sciences |
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| Online Access: | https://www.frontiersin.org/articles/10.3389/fspas.2023.1148293/full |
| _version_ | 1811159543784144896 |
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| author | Seth H. Garland Vasyl B. Yurchyshyn Robert D. Loper Benjamin F. Akers Daniel J. Emmons |
| author_facet | Seth H. Garland Vasyl B. Yurchyshyn Robert D. Loper Benjamin F. Akers Daniel J. Emmons |
| author_sort | Seth H. Garland |
| collection | DOAJ |
| description | The coronal magnetic field over NOAA Active Region 11,429 during a X5.4 solar flare on 7 March 2012 is modeled using optimization based Non-Linear Force-Free Field extrapolation. Specifically, 3D magnetic fields were modeled for 11 timesteps using the 12-min cadence Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager photospheric vector magnetic field data, spanning a time period of 1 hour before through 1 hour after the start of the flare. Using the modeled coronal magnetic field data, seven different magnetic field parameters were calculated for 3 separate regions: areas with surface |Bz|≥ 300 G, areas of flare brightening seen in SDO Atmospheric Imaging Assembly imagery, and areas with surface |B| ≥ 1000 G and high twist. Time series of the magnetic field parameters were analyzed to investigate the evolution of the coronal field during the solar flare event and discern pre-eruptive signatures. The data shows that areas with |B| ≥ 1000 G and |Tw|≥ 1.5 align well with areas of initial flare brightening during the pre-flare phase and at the beginning of the eruptive phase of the flare, suggesting that measurements of the photospheric magnetic field strength and twist can be used to predict the flare location within an active region if triggered. Additionally, the evolution of seven investigated magnetic field parameters indicated a destabilizing magnetic field structure that could likely erupt. |
| first_indexed | 2024-04-10T05:42:59Z |
| format | Article |
| id | doaj.art-3bca5713119844e8b32ae49e60f58853 |
| institution | Directory Open Access Journal |
| issn | 2296-987X |
| language | English |
| last_indexed | 2024-04-10T05:42:59Z |
| publishDate | 2023-03-01 |
| publisher | Frontiers Media S.A. |
| record_format | Article |
| series | Frontiers in Astronomy and Space Sciences |
| spelling | doaj.art-3bca5713119844e8b32ae49e60f588532023-03-06T05:50:53ZengFrontiers Media S.A.Frontiers in Astronomy and Space Sciences2296-987X2023-03-011010.3389/fspas.2023.11482931148293Evolution of coronal magnetic field parameters during X5.4 solar flareSeth H. Garland0Vasyl B. Yurchyshyn1Robert D. Loper2Benjamin F. Akers3Daniel J. Emmons4Department of Engineering Physics, Air Force Institute of Technology, Wright-Patterson AFB, OH, United StatesBig Bear Solar Observatory, New Jersey Institute of Technology, Big Bear, CA, United StatesMoon to Mars Space Weather Analysis Office, NASA Goddard Space Flight Center, Greenbelt, MD, United StatesDepartment of Mathematics and Statistics, Air Force Institute of Technology, Wright-Patterson AFB, OH, United StatesDepartment of Engineering Physics, Air Force Institute of Technology, Wright-Patterson AFB, OH, United StatesThe coronal magnetic field over NOAA Active Region 11,429 during a X5.4 solar flare on 7 March 2012 is modeled using optimization based Non-Linear Force-Free Field extrapolation. Specifically, 3D magnetic fields were modeled for 11 timesteps using the 12-min cadence Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager photospheric vector magnetic field data, spanning a time period of 1 hour before through 1 hour after the start of the flare. Using the modeled coronal magnetic field data, seven different magnetic field parameters were calculated for 3 separate regions: areas with surface |Bz|≥ 300 G, areas of flare brightening seen in SDO Atmospheric Imaging Assembly imagery, and areas with surface |B| ≥ 1000 G and high twist. Time series of the magnetic field parameters were analyzed to investigate the evolution of the coronal field during the solar flare event and discern pre-eruptive signatures. The data shows that areas with |B| ≥ 1000 G and |Tw|≥ 1.5 align well with areas of initial flare brightening during the pre-flare phase and at the beginning of the eruptive phase of the flare, suggesting that measurements of the photospheric magnetic field strength and twist can be used to predict the flare location within an active region if triggered. Additionally, the evolution of seven investigated magnetic field parameters indicated a destabilizing magnetic field structure that could likely erupt.https://www.frontiersin.org/articles/10.3389/fspas.2023.1148293/fullsolar coronasolar photospheresolar magnetic fieldactive regionsolar flaresNLFFF extrapolation |
| spellingShingle | Seth H. Garland Vasyl B. Yurchyshyn Robert D. Loper Benjamin F. Akers Daniel J. Emmons Evolution of coronal magnetic field parameters during X5.4 solar flare Frontiers in Astronomy and Space Sciences solar corona solar photosphere solar magnetic field active region solar flares NLFFF extrapolation |
| title | Evolution of coronal magnetic field parameters during X5.4 solar flare |
| title_full | Evolution of coronal magnetic field parameters during X5.4 solar flare |
| title_fullStr | Evolution of coronal magnetic field parameters during X5.4 solar flare |
| title_full_unstemmed | Evolution of coronal magnetic field parameters during X5.4 solar flare |
| title_short | Evolution of coronal magnetic field parameters during X5.4 solar flare |
| title_sort | evolution of coronal magnetic field parameters during x5 4 solar flare |
| topic | solar corona solar photosphere solar magnetic field active region solar flares NLFFF extrapolation |
| url | https://www.frontiersin.org/articles/10.3389/fspas.2023.1148293/full |
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