Multipoint study of the rapid filament evolution during a confined C2 flare on 28 March 2022, leading to eruption
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| Autores principales: | , , , , , , , |
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| Formato: | Preprint |
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2024
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| _version_ | 1866929416400011264 |
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| author | Purkhart, Stefan Veronig, Astrid M. Kliem, Bernhard Jarolim, Robert Dissauer, Karin Dickson, Ewan C. M. Podladchikova, Tatiana Krucker, Säm |
| author_facet | Purkhart, Stefan Veronig, Astrid M. Kliem, Bernhard Jarolim, Robert Dissauer, Karin Dickson, Ewan C. M. Podladchikova, Tatiana Krucker, Säm |
| contents | We studied the rapid filament evolution in AR 12975 during a confined C2 flare on 28 March 2022, which led to an eruptive M4 flare 1.5 h later. It is characterized by the breakup of the filament, the disappearance of its southern half, and the flow of the remaining plasma into a longer channel with a topology similar to an EUV hot channel during the flare. Our multipoint study takes advantage of Solar Orbiter's position at 0.33 AU and 83. 5° west of the Sun-Earth line. STIX and EUI onboard Solar Orbiter observed the event at the limb. AIA and HMI onboard SDO provided on-disk observations from which we derived DEM maps and NLFF magnetic field extrapolations. We find that both filament channels likely existed in close proximity before the flare. Based on field structures associated with AIA 1600 Å flare ribbons and kernels, we propose a loop-loop reconnection scenario between field lines that surround and pass beneath the shorter filament channel, and field lines following a portion of the longer channel. Reconnection occurs in an essentially vertical current sheet at a PIL below the breakup region, leading to the formation of the flare loop arcade and the EUV hot channel. The scenario is supported by concentrated currents and free magnetic energy built up by antiparallel flows along the PIL before the flare. The reconnection probably propagated to involve the original filament itself, leading to its breakup and reformation. The reconnection geometry provides a general mechanism for the formation of the long filament channel and realizes the concept of tether cutting, which was active throughout the filament's rise phase, lasting from at least 30 min before the C2 flare until the eruption. The C2 flare represents a period of fast reconnection during this otherwise more steady process, during which most of the original filament was reconnected and joined the longer channel. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_07777 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Multipoint study of the rapid filament evolution during a confined C2 flare on 28 March 2022, leading to eruption Purkhart, Stefan Veronig, Astrid M. Kliem, Bernhard Jarolim, Robert Dissauer, Karin Dickson, Ewan C. M. Podladchikova, Tatiana Krucker, Säm Solar and Stellar Astrophysics We studied the rapid filament evolution in AR 12975 during a confined C2 flare on 28 March 2022, which led to an eruptive M4 flare 1.5 h later. It is characterized by the breakup of the filament, the disappearance of its southern half, and the flow of the remaining plasma into a longer channel with a topology similar to an EUV hot channel during the flare. Our multipoint study takes advantage of Solar Orbiter's position at 0.33 AU and 83. 5° west of the Sun-Earth line. STIX and EUI onboard Solar Orbiter observed the event at the limb. AIA and HMI onboard SDO provided on-disk observations from which we derived DEM maps and NLFF magnetic field extrapolations. We find that both filament channels likely existed in close proximity before the flare. Based on field structures associated with AIA 1600 Å flare ribbons and kernels, we propose a loop-loop reconnection scenario between field lines that surround and pass beneath the shorter filament channel, and field lines following a portion of the longer channel. Reconnection occurs in an essentially vertical current sheet at a PIL below the breakup region, leading to the formation of the flare loop arcade and the EUV hot channel. The scenario is supported by concentrated currents and free magnetic energy built up by antiparallel flows along the PIL before the flare. The reconnection probably propagated to involve the original filament itself, leading to its breakup and reformation. The reconnection geometry provides a general mechanism for the formation of the long filament channel and realizes the concept of tether cutting, which was active throughout the filament's rise phase, lasting from at least 30 min before the C2 flare until the eruption. The C2 flare represents a period of fast reconnection during this otherwise more steady process, during which most of the original filament was reconnected and joined the longer channel. |
| title | Multipoint study of the rapid filament evolution during a confined C2 flare on 28 March 2022, leading to eruption |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2407.07777 |