Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
The first significant sunquake event of Solar Cycle 25 was observed during the X1.5 flare of 2022 May 10, by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory. We perform a detailed spectro-polarimetric analysis of the sunquake photospheric sources, using the Stokes...
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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/acf9eb |
| _version_ | 1827696343228874752 |
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| author | Alexander G. Kosovichev Viacheslav M. Sadykov John T. Stefan |
| author_facet | Alexander G. Kosovichev Viacheslav M. Sadykov John T. Stefan |
| author_sort | Alexander G. Kosovichev |
| collection | DOAJ |
| description | The first significant sunquake event of Solar Cycle 25 was observed during the X1.5 flare of 2022 May 10, by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory. We perform a detailed spectro-polarimetric analysis of the sunquake photospheric sources, using the Stokes profiles of the Fe i 6173 Å line, reconstructed from the HMI linear and circular polarized filtergrams. The results show fast variations of the continuum emission with rapid growth and slower decay lasting 3–4 minutes, coinciding in time with the hard X-ray impulses observed by the Konus instrument on board the Wind spacecraft. The variations in the line core appeared slightly ahead of the variations in the line wings, showing that the heating started in the higher atmospheric layers and propagated downward. The most significant feature of the line profile variations is the transient emission in the line core in three of the four sources, indicating intense, impulsive heating in the lower chromosphere and photosphere. In addition, the observed variations of the Stokes profiles reflect transient and permanent changes in the magnetic field strength and geometry in the sunquake sources. Comparison with the radiative hydrodynamics models shows that the physical processes in the impulsive flare phase are substantially more complex than those predicted by proton and electron beam flare models currently presented in the literature. |
| first_indexed | 2024-03-10T12:45:21Z |
| format | Article |
| id | doaj.art-398b0b3e59ed44ada12d489ed174ea92 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-10T12:45:21Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-398b0b3e59ed44ada12d489ed174ea922023-11-21T13:29:22ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01958216010.3847/1538-4357/acf9ebSpectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam ImpactsAlexander G. Kosovichev0https://orcid.org/0000-0003-0364-4883Viacheslav M. Sadykov1https://orcid.org/0000-0002-4001-1295John T. Stefan2https://orcid.org/0000-0002-5519-8291Department of Physics, New Jersey Institute of Technology , Newark, NJ 07102, USA ; alexander.g.kosovichev@njit.edu; NASA Ames Research Center , Moffett Field, Mountain View, CA 94040, USAPhysics & Astronomy Department, Georgia State University , Atlanta, GA 30303, USADepartment of Physics, New Jersey Institute of Technology , Newark, NJ 07102, USA ; alexander.g.kosovichev@njit.eduThe first significant sunquake event of Solar Cycle 25 was observed during the X1.5 flare of 2022 May 10, by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory. We perform a detailed spectro-polarimetric analysis of the sunquake photospheric sources, using the Stokes profiles of the Fe i 6173 Å line, reconstructed from the HMI linear and circular polarized filtergrams. The results show fast variations of the continuum emission with rapid growth and slower decay lasting 3–4 minutes, coinciding in time with the hard X-ray impulses observed by the Konus instrument on board the Wind spacecraft. The variations in the line core appeared slightly ahead of the variations in the line wings, showing that the heating started in the higher atmospheric layers and propagated downward. The most significant feature of the line profile variations is the transient emission in the line core in three of the four sources, indicating intense, impulsive heating in the lower chromosphere and photosphere. In addition, the observed variations of the Stokes profiles reflect transient and permanent changes in the magnetic field strength and geometry in the sunquake sources. Comparison with the radiative hydrodynamics models shows that the physical processes in the impulsive flare phase are substantially more complex than those predicted by proton and electron beam flare models currently presented in the literature.https://doi.org/10.3847/1538-4357/acf9ebSolar flaresSolar activitySolar active regions |
| spellingShingle | Alexander G. Kosovichev Viacheslav M. Sadykov John T. Stefan Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts The Astrophysical Journal Solar flares Solar activity Solar active regions |
| title | Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts |
| title_full | Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts |
| title_fullStr | Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts |
| title_full_unstemmed | Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts |
| title_short | Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts |
| title_sort | spectro polarimetric properties of sunquake sources in x1 5 flare and evidence for electron and proton beam impacts |
| topic | Solar flares Solar activity Solar active regions |
| url | https://doi.org/10.3847/1538-4357/acf9eb |
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