Multiwavelength Observations of the Formation and Eruption of a Complex Filament

Zhang, Y.; Bastian, T. S.; Liu, J. H.; Yu, Sijie; Feng, Song; Chen, Jie; Yan, Yihua

doi:10.3847/1538-4357/abded6

Cited by 8 publications

(12 citation statements)

References 71 publications

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“…Combining the observational results in the present study and previous study (Dhakal et al 2018;Zhang et al 2021), we suggest a physical scenario for the dynamic evolution of MFRs. A low-lying MFR-MFR1, which presents as filament, forms along the PIL more than 40 hr before the main eruption.…”

Section: Summary and Discussionsupporting

confidence: 86%

“…In the following, we will discuss the detail in four separate phases: (1) the long-term manifestation of MFR1, from March 09, 10:00 UT to March 10, 15:11 UT; (2) the dynamic evolution of MFR1 and MFR2, from 15:11 UT to 16:46 UT; (3) the formation of MFR3, from 16:46 UT to 17:17 UT; (4) the eruption of MFR3 and MFR4, for times later than 17:17 UT. Parts of the third and fourth processes are presented in Zhang et al (2021), but focused on the performance of filaments. Here we will present the dynamic evolution of the MFRs and associated features in details.…”

Section: Dynamic Evolution Of Mfrsmentioning

confidence: 99%

“…Meanwhile, it is also possible that there are no cool material deposited in dips of MFRs. Zhang et al (2021) suggest that the filament would form when coronal material gathered into a preexisting MFR. It is also observed that the erupting MFR does not accompany a preexisting filament (Li & Zhang 2013).…”

Section: Introductionmentioning

confidence: 99%

“…The AR 11429 is a highly flare-productive region (Elmhamdi et al 2014). Successive MFR eruptions from this AR were reported spanning almost the whole time period of its solar disk passage (Hao et al 2012;Chen et al 2014Chen et al , 2015Wang et al 2014;Chintzoglou et al 2015;Syntelis et al 2016;Dhakal et al 2018Dhakal et al , 2020Yang et al 2018;Zhou et al 2019Zhou et al , 2020Zhang et al 2021). Many aspects of the major eruption are also studied by numerous works.…”

Section: Introductionmentioning

confidence: 99%

“…Luo et al (2021) reported the signature of termination shock after Chen et al (2015) during the decay phase of the M8.4 flare. The formation and eruption of the filament, which is hosted by an MFR (here named MFR3), are presented by Zhang et al (2021). The observational evidences in their study demonstrate that the MFR3 is formed via the tether-cutting reconnection of two relatively small MFRs (MFR1 and MFR2), which locate along the PIL at the core region of AR 11429.…”

Section: Introductionmentioning

confidence: 99%

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Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. I. EUV Observations

Zhang¹,

Liu

Tan

et al. 2022

ApJ

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Studying the formation and dynamic evolution of the magnetic flux rope (MFR) is key to understanding the physics of most solar eruptions. In the present study, we investigate the dynamic evolution of four MFRs, which involve in a major eruption. The MFR1, which represents as filament (F1), first appears about 31 hr before the major eruption. The MFR2 appears as a hot-channel with a small filament (F2) in its east part. The hot-channel becomes intermittently visible about 2 hr before the major eruption. The MFR3 is formed by the reconnection between MFR1 and MFR2. The annular components of MFR3 along the MFR2 part appear as a hollow helical structure from the background with the temperature of several MK after the reconnection. Coronal material then flows along the hollow structure from MFR1 part to MFR2 part to form a new filament (F3), which is hosted by MFR3 and acts as the axial component of MFR3 in the following evolution. The MFR4 appears during MFR3's eruption phase as conjugated extreme ultraviolet (EUV) brightenings. Both brightenings extend outward into irregular ribbons with conjugate EUV dimmings inside. Meanwhile, an erupted hot-channel, which roots in the conjugated brightening, is identified. The morphology of the MFRs are also profiled by four associated flare ribbon pairs. The on-disk observations shed light on our understanding of the topology of the MFRs and their formation and eruption. Further work should lay emphasis on the magnetic environment for the MFR formation and evolution.

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Section: Summary and Discussionsupporting

confidence: 86%

Section: Dynamic Evolution Of Mfrsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. I. EUV Observations

Zhang¹,

Liu

Tan

et al. 2022

ApJ

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Transient dark ribbons at the outer boundaries of sunspot superpenumbrae in the chromosphere

Xu¹,

Zhang²

2023

A&A

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Context. Although the flow of material in sunspot superpenumbrae has been studied intensively, detailed observations about the evolution of material flow at the outer boundaries of sunspot superpenumbrae are rare. Aims. We study the evolution of the flow of material at the outer boundaries of superpenumbrae. Methods. Based on Hα observations from the New Vacuum Solar Telescope, we tracked the evolution of the flow of material at the outer boundaries of superpenumbrae in the chromosphere. Data from the Solar Dynamics Observatory Helioseismic Magnetic Imager were employed to examine the photospheric magnetic field environment relevant to the material flow. Results. We observed transient dark ribbons (TDRs) at the outer boundary of a sunspot superpenumbra in the chromosphere on 2018 May 12. The TDRs are located in the middle of the sunspot and a flocculus, and both of them have negative magnetic fields. While the ratio of the length and width of a TDR is greater than 8, we tracked the TDR from its formation to disappearance, so that six TDRs were studied in detail. Five TDRs were formed by the connection of several small dark sticks from end to end, and the sixth TDR was formed by the merging of two thin sticks. In the later stage of the TDR evolution, five TDRs were broken down into several small dark sticks, and the sixth TDR dissipated with oscillation. During the evolution process, no obvious flow of material along the TDRs is detected. Conclusions. We suggest that these TDRs are an observational representation of the regular aggregation of superpenumbral fibril footpoints and adjacent solar flocculus fibril footpoints at the outer boundaries of the sunspot superpenumbrae.

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A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734

Liu,

Zhang,

Zheng

et al. 2024

Universe

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We present a detailed analysis of a partial eruption of a sigmoid filament lying along the polarity inversion line (PIL) of the small active region (AR) NOAA 12734 (with an area of 1.44 ×103 square megameters). The active filament was rooted in a dipole sunspot of the AR. The eruption was associated with a C1.3 flare and subsequent large-scale coronal disturbances. During its solar disk passage before the flare, the AR had the following characteristics: (1) Most of the time, the magnetic field lines in the AR showed a sigmoidal structure (‘L1’) in the low corona and arc-shaped loops (i.e., ‘L2’) in the upper atmosphere. (2) An ‘X’-shaped structure was formed between the original ‘S’-shaped magnetic loop (‘L1’) and the newly rising one (‘L3’) between the main positive and negative magnetic polarities of the sunspots, and the intersection point of flux ropes ‘L1’ and ‘L3’ corresponds well with the area where the initial extreme-ultraviolet (EUV) 1600 Å brightening of the flare occurred. (3) The AR disobeyed the hemispherical helicity rule and had magnetic twist and writhe of the same signs, i.e., its magnetic helicity/current helicity were positive in the northern hemisphere. (4) Sustained magnetic emergence and cancellation occurred before the flare. Therefore, the magnetic reconnection of highly twisted helical flux ropes under the confinement of the overlying magnetic fields is probably responsible for the partial eruption of the filament.

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Multiwavelength Observations of the Formation and Eruption of a Complex Filament

Cited by 8 publications

References 71 publications

Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. I. EUV Observations

Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. I. EUV Observations

Transient dark ribbons at the outer boundaries of sunspot superpenumbrae in the chromosphere

A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734

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