Observation of a Large-scale Quasi-circular Secondary Ribbon Associated with Successive Flares and a Halo CME

Lim, Eun-Kyung; Yurchyshyn, Vasyl; Kumar, Pankaj; Cho, Kyuhyoun; Jiang, Chaowei; Kim, S.; Yang, Heesu; Chae, Jongchul; Cho, Kyung-Suk; Lee, Jeongwoo

doi:10.3847/1538-4357/aa93f7

Cited by 11 publications

(10 citation statements)

References 44 publications

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“…Slipping motion of flare ribbons were not only observed in circular flare ribbons (e.g., Masson et al 2009;Liu et al 2013;Jiang et al 2015;Romano et al 2017;Lim et al 2017;Li et al 2018), but also in many other kinds of flare ribbons (e.g., Dudík et al 2014Dudík et al , 2016Li et al 2016;Zheng et al 2016;Lörinčík et al 2019). The slipping speeds reported in previous studies are ranged from 30 to 450 km s −1 .…”

Section: Conclusion and Discussionmentioning

confidence: 92%

“…So far, only one study reported the round-trip slipping motion along the inner flare ribbon (Wang & Liu 2012). The slipping motion of circular flare ribbons towards a certain direction have been observed in a few cases (e.g., Masson et al 2009;Liu et al 2013;Jiang et al 2015;Romano et al 2017;Lim et al 2017;Li et al 2018), but round-trip slipping motion of circular flare ribbon has not been reported yet.…”

Section: Introductionmentioning

confidence: 99%

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Round-trip Slipping Motion of the Circular Flare Ribbon Evidenced in a Fan-spine Jet

Shen

Zhou

et al. 2019

ApJL

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A solar jet on 2014 July 31, which was accompanied by a GOES C1.3 flare and a mini-filament eruption at the jet base, was studied by using observations taken by the New Vacuum Solar Telescope and the Solar Dynamic Observatory. Magnetic field extrapolation revealed that the jet was confined in a fan-spine magnetic system that hosts a null point at the height of about 9 Mm from the solar surface. An inner flare ribbon surrounded by an outer circular ribbon and a remote ribbon were observed to be associated with the eruption, in which the inner and remote ribbons respectively located at the footprints of the inner and outer spines, while the circular one manifested the footprint of the fan structure. It is interesting that the circular ribbon's west part showed an interesting round-trip slipping motion, while the inner ribbon and the circular ribbon's east part displayed a northward slipping motion. Our analysis results indicate that the slipping motions of the inner and the circular flare ribbons reflected the slipping magnetic reconnection process in the fan quasi-separatrix layer, while the remote ribbon was associated with the magnetic reconnection at the null point. In addition, the filament eruption was probably triggered by the magnetic cancellation around its south end, which further drove the slipping reconnection in the fan quasiseparatrix layer and the reconnection at the null point.

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Section: Conclusion and Discussionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Round-trip Slipping Motion of the Circular Flare Ribbon Evidenced in a Fan-spine Jet

Shen

Zhou

et al. 2019

ApJL

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“…Although the fan-spine morphology has been extensively investigated, the previous studies are mainly dedicated to the formation and changes of magnetic configuration and the associated explosive events (e.g., Guglielmino et al 2010;Jiang et al 2015;Yang et al 2015c;Lim et al 2017;Kumar et al 2019), and there is no simultaneous imaging and spectral study on the null point during solar flare. In this paper, we study a fan-spine structure in active region (AR) 12736 on 2019 March 22, and focus on the null point where magnetic reconnection occurred during a B6.7 flare, combing the high-quality vector magnetograms from the Hinode (Kosugi et al 2007) with the high-resolution imaging and spectral observations from the New Vacuum Solar Telescope (NVST; Liu et al 2014), the Solar Dynamics Observatory (SDO; Pesnell et al 2012), and the Interface Region Imaging Spectrograph (IRIS ; De Pontieu et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Imaging and spectral study on the null point of a fan-spine structure during a solar flare

Yang,

Zhang,

et al. 2020

Preprint

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Using the multi-instrument observations, we make the first simultaneous imaging and spectral study on the null point of a fan-spine magnetic topology during a solar flare. When magnetic reconnection occurs at the null point, the fan-spine configuration brightens in the (extreme-)ultraviolet channels. In the Hα images, the fan-spine structure is partly filled and outlined by the bi-directional material flows ejected from the reconnection site. The extrapolated coronal magnetic field confirms the existence of the fan-spine topology. Before and after the flare peak, the total velocity of the outflows is estimated to be about 60 km s −1 . During the flare, the Si iv line profile at the reconnection region is enhanced both in the blue-wing and red-wing. At the flare peak time, the total velocity of the outflows is found to be 144 km s −1 . Superposed on the Si iv profile, there are several deep absorption lines with the blueshift of several tens of km s −1 . The reason is inferred to be that the bright reconnection region observed in Si iv channel is located under the cooler material appearing as dark features in the Hα line. The blueshifted absorption lines indicate the movement of the cooler material toward the observer. The depth of the absorption lines also depends on the amount of cooler material. These results imply that this kind of spectral

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“…In a circular ribbon flare, null-point reconnection occurs and accelerates particles, which subsequently flow along the separatrix surface and the spine field into the lower atmosphere. As a result, the circular ribbon is formed at the intersection of the dome-shaped fan and the lower atmosphere (Hao et al 2017;Masson et al 2017;Xu et al 2017;Lim et al 2017). When the outer spine field is connected to a remote field, a remote brightening ribbon would appear (Reid et al 2012;Li et al 2017a;Hernandez-Perez et al 2017).…”

Section: Introductionmentioning

confidence: 99%

A Secondary Fan-spine Magnetic Structure in Active Region 11897

Hou

Yang

et al. 2019

ApJ

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Fan-spine is a special topology in solar atmosphere and is closely related to magnetic null point as well as circular-ribbon flares, which can provide important information for understanding the intrinsic three-dimensional (3D) nature of solar flares. However, the fine structure within the fan has rarely been investigated. In present paper, we investigate a secondary fan-spine (SFS) structure within the fan of a larger fan-spine topology. On 2013 November 18, this large fan-spine structure was traced out due to the partial eruption of a filament, which caused a circular-ribbon flare in active region 11897. The extrapolated 3D magnetic fields and squashing factor Q maps depict distinctly this fan-spine topology, its surrounding quasi-separatrix layer (QSL) halo, and a smaller quasi-circular ribbon with high Q located in the center, which implies the existence of fine structure within the fan. The imaging observations, extrapolated 3D fields, and Q maps on November 17 show that there indeed exists an SFS surrounded by a QSL, which is enveloped by another QSL-halo corresponding to the overlying larger domeshaped fan. Moreover, the material flows caused by the null-point reconnection are also detected along this SFS. After checking the evolution of the underneath magnetic fields, we suggest that the continuous emergence of magnetic flux within the central parasitic region encompassed by the opposite-polarity fields results in the formation of the SFS under the large fan.

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Observation of a Large-scale Quasi-circular Secondary Ribbon Associated with Successive Flares and a Halo CME

Cited by 11 publications

References 44 publications

Round-trip Slipping Motion of the Circular Flare Ribbon Evidenced in a Fan-spine Jet

Round-trip Slipping Motion of the Circular Flare Ribbon Evidenced in a Fan-spine Jet

Imaging and spectral study on the null point of a fan-spine structure during a solar flare

A Secondary Fan-spine Magnetic Structure in Active Region 11897

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