A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons
We analyze high-cadence vector magnetograms (135 s) and flare-ribbon observations of 37 flares from the Solar Dynamics Observatory to understand the spatial and temporal properties of changes in the photospheric vector magnetic field and their relationship to footpoints of reconnected fields. Confir...
| 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/acaa9d |
| _version_ | 1797697189335531520 |
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| author | Rahul Yadav M. D. Kazachenko |
| author_facet | Rahul Yadav M. D. Kazachenko |
| author_sort | Rahul Yadav |
| collection | DOAJ |
| description | We analyze high-cadence vector magnetograms (135 s) and flare-ribbon observations of 37 flares from the Solar Dynamics Observatory to understand the spatial and temporal properties of changes in the photospheric vector magnetic field and their relationship to footpoints of reconnected fields. Confirming previous studies, we find that the largest permanent changes in the horizontal field component lie near the polarity inversion line, whereas changes in the vertical field are less pronounced and are distributed throughout the active region. We find that pixels swept up by ribbons do not always exhibit permanent changes in the field. However, when they do, ribbon emission typically occurs several minutes before the start time of field changes. The changes in the properties of the field show no relation to the size of active regions, but are strongly related to the flare-ribbon properties such as ribbon magnetic flux and ribbon area. For the first time, we find that the duration of permanent changes in the field is strongly coupled with the duration of the flare, lasting on average 29% of the duration of the GOES flare. Our results suggest that changes in photospheric magnetic fields are caused by a combination of two scenarios: contraction of flare loops driven by magnetic reconnection and coronal implosion. |
| first_indexed | 2024-03-12T03:36:42Z |
| format | Article |
| id | doaj.art-63520caab6304644af501e6772e0fc09 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:36:42Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-63520caab6304644af501e6772e0fc092023-09-03T13:08:35ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01944221510.3847/1538-4357/acaa9dA Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare RibbonsRahul Yadav0https://orcid.org/0000-0003-4065-0078M. D. Kazachenko1https://orcid.org/0000-0001-8975-7605Laboratory for Atmospheric and Space Physics, University of Colorado Boulder , Boulder, CO 80303, USA ; rahul.yadav@lasp.colorado.eduLaboratory for Atmospheric and Space Physics, University of Colorado Boulder , Boulder, CO 80303, USA ; rahul.yadav@lasp.colorado.edu; National Solar Observatory , 3665 Discovery Drive, Boulder, CO 80303, USA; Department of Astrophysical and Planetary Sciences, University of Colorado Boulder , 2000 Colorado Avenue, Boulder, CO 80305, USAWe analyze high-cadence vector magnetograms (135 s) and flare-ribbon observations of 37 flares from the Solar Dynamics Observatory to understand the spatial and temporal properties of changes in the photospheric vector magnetic field and their relationship to footpoints of reconnected fields. Confirming previous studies, we find that the largest permanent changes in the horizontal field component lie near the polarity inversion line, whereas changes in the vertical field are less pronounced and are distributed throughout the active region. We find that pixels swept up by ribbons do not always exhibit permanent changes in the field. However, when they do, ribbon emission typically occurs several minutes before the start time of field changes. The changes in the properties of the field show no relation to the size of active regions, but are strongly related to the flare-ribbon properties such as ribbon magnetic flux and ribbon area. For the first time, we find that the duration of permanent changes in the field is strongly coupled with the duration of the flare, lasting on average 29% of the duration of the GOES flare. Our results suggest that changes in photospheric magnetic fields are caused by a combination of two scenarios: contraction of flare loops driven by magnetic reconnection and coronal implosion.https://doi.org/10.3847/1538-4357/acaa9dSolar flaresSolar magnetic fieldsThe Sun |
| spellingShingle | Rahul Yadav M. D. Kazachenko A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons The Astrophysical Journal Solar flares Solar magnetic fields The Sun |
| title | A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons |
| title_full | A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons |
| title_fullStr | A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons |
| title_full_unstemmed | A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons |
| title_short | A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons |
| title_sort | statistical analysis of magnetic field changes in the photosphere during solar flares using high cadence vector magnetograms and their association with flare ribbons |
| topic | Solar flares Solar magnetic fields The Sun |
| url | https://doi.org/10.3847/1538-4357/acaa9d |
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