Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the Sun
Remote brightening (RB) is compact brightening at footpoints of magnetic loops, which are remotely connecting to and confining an eruption in the solar atmosphere. Here, we report on observations of an RB resulting from an EUV jet with a speed of about 90 km s ^−1 . The loops connecting the RB and t...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada444 |
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| author | Chao Zhang Zhenghua Huang Hengyuan Wei Youqian Qi Mijie Shi Hui Fu Xiuhui Zuo Weixin Liu Mingzhe Sun Ming Xiong Lidong Xia |
| author_facet | Chao Zhang Zhenghua Huang Hengyuan Wei Youqian Qi Mijie Shi Hui Fu Xiuhui Zuo Weixin Liu Mingzhe Sun Ming Xiong Lidong Xia |
| author_sort | Chao Zhang |
| collection | DOAJ |
| description | Remote brightening (RB) is compact brightening at footpoints of magnetic loops, which are remotely connecting to and confining an eruption in the solar atmosphere. Here, we report on observations of an RB resulting from an EUV jet with a speed of about 90 km s ^−1 . The loops connecting the RB and the jet have an apparent length of about 59 Mm. Intriguingly, the RB exhibits at least two episodes of brightenings, as characterized by two peaks in its lightcurve. The energies that sustain the first and second peaks of the RB are 6.3 × 10 ^26 erg and 8.4 × 10 ^26 erg, respectively, and comprise a significant proportion of the total energy. The first peak of the RB brightenings coincides with the jet's peak with a time delay of 12 s, while the second peak lags behind by 108 s. Besides the flows of the ejecta, we have identified two additional flows originating from the eruption site. One is relatively cool with a temperature of ${{\rm{log}}}_{10}(T/{\rm{K}})=5.8$ –6.1 and a speed of about 275 ± 15 km s ^−1 . The other is hot with a temperature of ${{\rm{log}}}_{10}(T/{\rm{K}})=7.0$ –7.3 and a much greater speed of about 750 ± 70 km s ^−1 . We attribute the second peak of RB directly to this hot flow, which our numerical experiments suggest is the result of a slow shock wave. Considering the minimal time delay between the first peak of RB and the eruption, we infer that this first episode is due to heating by nonthermal electrons. Our research demonstrates that the dynamics in an RB can offer vital insights into the nature of the corresponding eruption and help understand how energy is distributed throughout the solar atmosphere. |
| format | Article |
| id | doaj-art-3c7f03ea0e16445194ce8114b2518b23 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-3c7f03ea0e16445194ce8114b2518b232025-01-27T07:04:00ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01979218010.3847/1538-4357/ada444Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the SunChao Zhang0Zhenghua Huang1https://orcid.org/0000-0002-2358-5377Hengyuan Wei2https://orcid.org/0000-0002-0210-6365Youqian Qi3Mijie Shi4https://orcid.org/0000-0002-9201-5896Hui Fu5https://orcid.org/0000-0002-8827-9311Xiuhui Zuo6Weixin Liu7Mingzhe Sun8https://orcid.org/0000-0002-1631-9898Ming Xiong9https://orcid.org/0000-0001-9427-7366Lidong Xia10https://orcid.org/0000-0001-8938-1038Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of ChinaShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of ChinaShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnKey Laboratory of Solar Activity and Space Weather, National Space Science Center , Chinese Academy of Sciences, Beijing 100190, People’s Republic of China; College of Earth and Planetary Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University , Weihai 264209, Shandong, People’s Republic of China ; z.huang@sdu.edu.cnRemote brightening (RB) is compact brightening at footpoints of magnetic loops, which are remotely connecting to and confining an eruption in the solar atmosphere. Here, we report on observations of an RB resulting from an EUV jet with a speed of about 90 km s ^−1 . The loops connecting the RB and the jet have an apparent length of about 59 Mm. Intriguingly, the RB exhibits at least two episodes of brightenings, as characterized by two peaks in its lightcurve. The energies that sustain the first and second peaks of the RB are 6.3 × 10 ^26 erg and 8.4 × 10 ^26 erg, respectively, and comprise a significant proportion of the total energy. The first peak of the RB brightenings coincides with the jet's peak with a time delay of 12 s, while the second peak lags behind by 108 s. Besides the flows of the ejecta, we have identified two additional flows originating from the eruption site. One is relatively cool with a temperature of ${{\rm{log}}}_{10}(T/{\rm{K}})=5.8$ –6.1 and a speed of about 275 ± 15 km s ^−1 . The other is hot with a temperature of ${{\rm{log}}}_{10}(T/{\rm{K}})=7.0$ –7.3 and a much greater speed of about 750 ± 70 km s ^−1 . We attribute the second peak of RB directly to this hot flow, which our numerical experiments suggest is the result of a slow shock wave. Considering the minimal time delay between the first peak of RB and the eruption, we infer that this first episode is due to heating by nonthermal electrons. Our research demonstrates that the dynamics in an RB can offer vital insights into the nature of the corresponding eruption and help understand how energy is distributed throughout the solar atmosphere.https://doi.org/10.3847/1538-4357/ada444Solar coronaSolar coronal transientsSolar coronal loopsSolar coronal heatingSolar atmosphereSolar magnetic fields |
| spellingShingle | Chao Zhang Zhenghua Huang Hengyuan Wei Youqian Qi Mijie Shi Hui Fu Xiuhui Zuo Weixin Liu Mingzhe Sun Ming Xiong Lidong Xia Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the Sun The Astrophysical Journal Solar corona Solar coronal transients Solar coronal loops Solar coronal heating Solar atmosphere Solar magnetic fields |
| title | Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the Sun |
| title_full | Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the Sun |
| title_fullStr | Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the Sun |
| title_full_unstemmed | Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the Sun |
| title_short | Multiple Episodes of Remote Brightenings Driven by a Coronal Extreme-ultraviolet Jet on the Sun |
| title_sort | multiple episodes of remote brightenings driven by a coronal extreme ultraviolet jet on the sun |
| topic | Solar corona Solar coronal transients Solar coronal loops Solar coronal heating Solar atmosphere Solar magnetic fields |
| url | https://doi.org/10.3847/1538-4357/ada444 |
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