Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament Channel
Similar to the cases of anemone jets, two-sided loop solar jets can also be produced by either flux emergence from the solar interior or small-scale filament eruptions. Using high-quality data from the Solar Dynamics Observatory, we have analyzed a two-sided loop solar jet triggered by the eruption...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad23e5 |
| _version_ | 1797266087429013504 |
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| author | Jiayan Yang Hechao Chen Junchao Hong Bo Yang Yi Bi |
| author_facet | Jiayan Yang Hechao Chen Junchao Hong Bo Yang Yi Bi |
| author_sort | Jiayan Yang |
| collection | DOAJ |
| description | Similar to the cases of anemone jets, two-sided loop solar jets can also be produced by either flux emergence from the solar interior or small-scale filament eruptions. Using high-quality data from the Solar Dynamics Observatory, we have analyzed a two-sided loop solar jet triggered by the eruption of a small filament. The jet occurred in a pre-existing big filament channel. The detailed processes involved in the eruption of the small filament, the interaction between the erupted filament and the big filament channel, and the launch of the two-sided loop jet are presented. The observations further revealed notable asymmetry between the two branches of the jet spire: the northeastern branch is narrow and short, while the southern branch is wide and long and accompanied by discernible untwisting motions. We explored the unique appearance of the jet by employing the method of local potential field extrapolation to calculate the coronal magnetic field configuration around the jet. The photospheric magnetic flux below the small filament underwent cancellation for approximately 7 hr before the filament eruption, and the negative flux near the southern footpoint of the filament decreased by about 56% during this interval. Therefore, we propose that the primary photospheric driver of the filament eruption and the associated two-sided loop jet in this event is flux cancellation rather than flux emergence. |
| first_indexed | 2024-04-25T00:55:07Z |
| format | Article |
| id | doaj.art-853637f15aa74f1b983a023d24b9ad9c |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-25T00:55:07Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj.art-853637f15aa74f1b983a023d24b9ad9c2024-03-11T11:26:16ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-019641710.3847/1538-4357/ad23e5Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament ChannelJiayan Yang0https://orcid.org/0000-0003-3462-4340Hechao Chen1https://orcid.org/0000-0001-7866-4358Junchao Hong2Bo Yang3Yi Bi4https://orcid.org/0000-0002-5302-3404Yunnan Observatory, Chinese Academy of Sciences , P.O. Box 110, Kunming 650011, People's Republic of ChinaSchool of Physics and Astronomy, Yunnan University , Kunming 650500, People's Republic of ChinaYunnan Observatory, Chinese Academy of Sciences , P.O. Box 110, Kunming 650011, People's Republic of ChinaYunnan Observatory, Chinese Academy of Sciences , P.O. Box 110, Kunming 650011, People's Republic of China; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650011, People's Republic of ChinaYunnan Observatory, Chinese Academy of Sciences , P.O. Box 110, Kunming 650011, People's Republic of China; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650011, People's Republic of ChinaSimilar to the cases of anemone jets, two-sided loop solar jets can also be produced by either flux emergence from the solar interior or small-scale filament eruptions. Using high-quality data from the Solar Dynamics Observatory, we have analyzed a two-sided loop solar jet triggered by the eruption of a small filament. The jet occurred in a pre-existing big filament channel. The detailed processes involved in the eruption of the small filament, the interaction between the erupted filament and the big filament channel, and the launch of the two-sided loop jet are presented. The observations further revealed notable asymmetry between the two branches of the jet spire: the northeastern branch is narrow and short, while the southern branch is wide and long and accompanied by discernible untwisting motions. We explored the unique appearance of the jet by employing the method of local potential field extrapolation to calculate the coronal magnetic field configuration around the jet. The photospheric magnetic flux below the small filament underwent cancellation for approximately 7 hr before the filament eruption, and the negative flux near the southern footpoint of the filament decreased by about 56% during this interval. Therefore, we propose that the primary photospheric driver of the filament eruption and the associated two-sided loop jet in this event is flux cancellation rather than flux emergence.https://doi.org/10.3847/1538-4357/ad23e5Solar activitySolar filament eruptionsSolar magnetic fields |
| spellingShingle | Jiayan Yang Hechao Chen Junchao Hong Bo Yang Yi Bi Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament Channel The Astrophysical Journal Solar activity Solar filament eruptions Solar magnetic fields |
| title | Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament Channel |
| title_full | Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament Channel |
| title_fullStr | Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament Channel |
| title_full_unstemmed | Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament Channel |
| title_short | Two-sided Loop Solar Jet Driven by the Eruption of a Small Filament in a Big Filament Channel |
| title_sort | two sided loop solar jet driven by the eruption of a small filament in a big filament channel |
| topic | Solar activity Solar filament eruptions Solar magnetic fields |
| url | https://doi.org/10.3847/1538-4357/ad23e5 |
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