High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons
We analyze high-resolution observations of an X-1.0 white-light flare, triggered by a filament eruption, on 2022 October 2. The full process of filament formation and subsequent eruption was captured in the H α passband by the Visible Imaging Spectrograph (VIS) on board the Goode Solar Telescope (GS...
Saved in:
| Main Authors: | , , , , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
|
| Series: | The Astrophysical Journal Letters |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/2041-8213/ada9e4 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1832582453997338624 |
|---|---|
| author | Xu Yang Meiqi Wang Andrew Cao Kaifan Ji Vasyl Yurchyshyn Jiong Qiu Sijie Yu Jinhua Shen Wenda Cao |
| author_facet | Xu Yang Meiqi Wang Andrew Cao Kaifan Ji Vasyl Yurchyshyn Jiong Qiu Sijie Yu Jinhua Shen Wenda Cao |
| author_sort | Xu Yang |
| collection | DOAJ |
| description | We analyze high-resolution observations of an X-1.0 white-light flare, triggered by a filament eruption, on 2022 October 2. The full process of filament formation and subsequent eruption was captured in the H α passband by the Visible Imaging Spectrograph (VIS) on board the Goode Solar Telescope (GST) within its center field of view. White-light emissions appear in flare ribbons following the filament eruption and H α ribbon brightening. GST Broadband Filter Imager data show that the continuum intensity, as compared to the nearby quiet-Sun area, has increased by up to 20% in the photospheric TiO band around 7057 Å. The Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory reported 10% contrast enhancement in the continuum near Fe i 6173 Å line. The separation motion of two white-light kernels is recorded by the high-cadence GST/TiO images and is well accompanied by the motion of the VIS H α flare ribbon leading edge. One kernel, located in a 150 Gauss field within a granulation area, exhibited an average apparent motion speed of 55 km s ^−1 , which is the highest average speed ever reported. The other kernel drifted at 9 km s ^−1 in an 800 Gauss magnetic field area. Hard X-ray (HXR) emissions reaching up to 300 keV have been observed for this flare. The simultaneous occurrence of high-cadence HXR, microwave, and white-light emissions strongly suggests that the energetic particles from the flare directly contribute to the heating. The inverted HXR energy flux density corresponding to 10% TiO brightening is 2.07 ± 0.23 × 10 ^11 erg cm ^−2 s ^−1 during the flare peak. |
| format | Article |
| id | doaj-art-72d5341c5dc34b49a79ded61054c8393 |
| institution | Kabale University |
| issn | 2041-8205 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj-art-72d5341c5dc34b49a79ded61054c83932025-01-29T18:02:24ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019792L4310.3847/2041-8213/ada9e4High-resolution Observations of an X-1.0 White-light Flare with Moving Flare RibbonsXu Yang0https://orcid.org/0000-0002-3238-0779Meiqi Wang1https://orcid.org/0000-0002-2633-3562Andrew Cao2https://orcid.org/0009-0004-3700-4440Kaifan Ji3https://orcid.org/0000-0001-8950-3875Vasyl Yurchyshyn4https://orcid.org/0000-0001-9982-2175Jiong Qiu5https://orcid.org/0000-0002-2797-744XSijie Yu6https://orcid.org/0000-0003-2872-2614Jinhua Shen7https://orcid.org/0000-0003-4439-4972Wenda Cao8https://orcid.org/0000-0003-2427-6047Big Bear Solar Observatory , 40386 N Shore Ln., Big Bear, CA 92314, USA ; Xu.Yang@njit.edu, wenda.cao@njit.eduCenter for Solar-Terrestrial Research, New Jersey Institute of Technology , 323 Martin Luther King Jr Blvd., Newark, NJ 07102-1982, USAUnion County Vocational-Technical Schools , 1776 Raritan Rd., Scotch Plains, NJ 07076, USAYunnan Observatories, Chinese Academy of Sciences , 396 Yangfangwang, Kunming, Yunnan 650011, People’s Republic of ChinaBig Bear Solar Observatory , 40386 N Shore Ln., Big Bear, CA 92314, USA ; Xu.Yang@njit.edu, wenda.cao@njit.eduDepartment of Physics, Montana State University , Bozeman, MT 59717, USACenter for Solar-Terrestrial Research, New Jersey Institute of Technology , 323 Martin Luther King Jr Blvd., Newark, NJ 07102-1982, USAXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of ChinaBig Bear Solar Observatory , 40386 N Shore Ln., Big Bear, CA 92314, USA ; Xu.Yang@njit.edu, wenda.cao@njit.edu; Center for Solar-Terrestrial Research, New Jersey Institute of Technology , 323 Martin Luther King Jr Blvd., Newark, NJ 07102-1982, USAWe analyze high-resolution observations of an X-1.0 white-light flare, triggered by a filament eruption, on 2022 October 2. The full process of filament formation and subsequent eruption was captured in the H α passband by the Visible Imaging Spectrograph (VIS) on board the Goode Solar Telescope (GST) within its center field of view. White-light emissions appear in flare ribbons following the filament eruption and H α ribbon brightening. GST Broadband Filter Imager data show that the continuum intensity, as compared to the nearby quiet-Sun area, has increased by up to 20% in the photospheric TiO band around 7057 Å. The Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory reported 10% contrast enhancement in the continuum near Fe i 6173 Å line. The separation motion of two white-light kernels is recorded by the high-cadence GST/TiO images and is well accompanied by the motion of the VIS H α flare ribbon leading edge. One kernel, located in a 150 Gauss field within a granulation area, exhibited an average apparent motion speed of 55 km s ^−1 , which is the highest average speed ever reported. The other kernel drifted at 9 km s ^−1 in an 800 Gauss magnetic field area. Hard X-ray (HXR) emissions reaching up to 300 keV have been observed for this flare. The simultaneous occurrence of high-cadence HXR, microwave, and white-light emissions strongly suggests that the energetic particles from the flare directly contribute to the heating. The inverted HXR energy flux density corresponding to 10% TiO brightening is 2.07 ± 0.23 × 10 ^11 erg cm ^−2 s ^−1 during the flare peak.https://doi.org/10.3847/2041-8213/ada9e4Solar white-light flaresSolar filament eruptionsSolar photosphereSolar chromosphere |
| spellingShingle | Xu Yang Meiqi Wang Andrew Cao Kaifan Ji Vasyl Yurchyshyn Jiong Qiu Sijie Yu Jinhua Shen Wenda Cao High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons The Astrophysical Journal Letters Solar white-light flares Solar filament eruptions Solar photosphere Solar chromosphere |
| title | High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons |
| title_full | High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons |
| title_fullStr | High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons |
| title_full_unstemmed | High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons |
| title_short | High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons |
| title_sort | high resolution observations of an x 1 0 white light flare with moving flare ribbons |
| topic | Solar white-light flares Solar filament eruptions Solar photosphere Solar chromosphere |
| url | https://doi.org/10.3847/2041-8213/ada9e4 |
| work_keys_str_mv | AT xuyang highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT meiqiwang highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT andrewcao highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT kaifanji highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT vasylyurchyshyn highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT jiongqiu highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT sijieyu highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT jinhuashen highresolutionobservationsofanx10whitelightflarewithmovingflareribbons AT wendacao highresolutionobservationsofanx10whitelightflarewithmovingflareribbons |