Velocities of Flare Kernels and the Mapping Norm of Field Line Connectivity

Lörinčík, Juraj; Aulanier, G.; Dudík, J.; Zemanová, Alena; Dzifčáková, E.

doi:10.3847/1538-4357/ab298f

Cited by 17 publications

(29 citation statements)

References 61 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%

“…Converging and separation motions of conjugated flare two ribbons are perpendicular to the magnetic neutral line, and they are interpreted to be manifestations of the downward and upward motions of the reconnection sites (e.g., Ji et al 2006). Slipping motions are along flare ribbons, which manifest the slipping magnetic reconnection process within QSLs (Aulanier et al 2006;Dudík et al 2014Dudík et al , 2016Zheng et al 2016;Li et al 2016Li et al , 2018Lörinčík et al 2019). For fan-spine magnetic topologies, the flare ribbons at different locations are caused by energetic particle beams along different magnetic loops as mention above (Reid et al 2012).…”

Section: Introductionmentioning

confidence: 97%

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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: 97%

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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“…While the standard aa-rf reconnection has been observed in several events either as coronal inflows (e.g., Yokoyama et al 2001;Zhu et al 2016) or as apparently slipping flare loops (e.g., Dudík et al 2014), the only evidence for ar-rf reconnection as presented in relied only on ribbon deformation. In the works of Zemanova et al (2019) and Lörinčík et al (2019), the evidence was incomplete, as only some of the four components of the ar-rf reconnection were visible. In Lörinčík et al (2019), footpoints of an erupting filament were swept by the ribbon hook and turned to flare loops, a signature of the ar-rf reconnection.…”

Section: Introductionmentioning

confidence: 99%

Observation of All Pre- and Post-reconnection Structures Involved in Three-dimensional Reconnection Geometries in Solar Eruptions

Dudík

Lörinčík

Aulanier

et al. 2019

ApJ

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We report on observations of the two newly-identified reconnection geometries involving erupting flux ropes. In 3D, a flux rope can reconnect either with a surrounding coronal arcade (recently named "ar-rf" reconnection) or with itself ("rr-rf" reconnection), and both kinds of reconnection create a new flux rope field line and a flare loop. For the first time, we identify all four constituents of both reconnections in a solar eruptive event, the filament eruption of 2011 June 07 observed by SDO/AIA. The ar-rf reconnection manifests itself as shift of one leg of the filament by more than 25 northward. At its previous location, a flare arcade is formed, while the new location of the filament leg previously corresponded to a footpoint of a coronal loop in 171Å. In addition, the evolution of the flare ribbon hooks is also consistent with the occurrence of ar-rf reconnection as predicted by MHD simulations. Specifically, the growing hook sweeps footpoints of preeruptive coronal arcades, and these locations become inside the hook. Furthermore, the rr-rf reconnection occurs during the peak phase above the flare arcade, in an apparently X-type geometry involving a pair of converging bright filament strands in the erupting filament. A new flare loop forms near the leg of one of the strands, while a bright blob, representing a remnant of the same strand, is seen ascending into the erupting filament. All together, these observations vindicate recent predictions of the 3D standard solar flare model.

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“…The VCS must be a three-dimensional structure, which is implied by the post-flare arcade. However, it may not be a continuous "slab", extending continuously along the axis of the postflare arcade, because 1) the arcade consists of numerous discrete post-flare loops (e.g., Jing et al 2016); 2) the flare ribbons, which are the footpoints of post-flare loops, often consist of discrete kernels in Hα and UV (e.g., Li & Zhang 2015;Lörinčík et al 2019); and 3) the supra-arcade fan is far from uniform but the haze-like plasma is often superimposed by multiple spike-like features (e.g, Figure 1(e & f)), which are discretely aligned along the top of the arcade and termed supra-arcade spikes (SASs) in this paper. If a post-flare arcade is viewed from an LOS along its axis and there are no prominent coronal features in the foreground or background along the LOS, then the resultant supra-arcade emission must be integrated over the aligned SASs, which gives a linear bright feature extending vertically above the top of the arcade, i.e., a typical VCS (e.g., Liu et al 2010;Cheng et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Investigation on the Spatiotemporal Structures of Supra-Arcade Spikes

Liu,

Wang

2021

Preprint

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Context. The vertical current sheet (VCS) trailing coronal mass ejections (CMEs) is the key place where the flare energy release and the CME buildup take place through magnetic reconnection. It is often studied from the edge-on perspective for the morphological similarity with the two-dimensional "standard" picture, but its three dimensional structure can only be revealed when the flare arcade is observed side on. The structure and dynamics in the so-called supra-arcade region thus contain important clues to the physical processes in flares and CMEs.Aims. Here we focus on the supra-arcade spikes (SASs), interpreted as the VCS viewed side-on, to study their spatiotemporal structures. By comparing the number of spikes and the in-situ derived magnetic twist in interplanetary CMEs (ICMEs), we intend to check on the inference from the standard picture that each spike represents an active reconnection site, with each episode of reconnection adding approximately one turn of twist to the CME flux rope. Methods. For this investigation we selected four events, in which the flare arcade has a significant north-south orientation and the associated CME is traversed by a near-Earth spacecraft. We studied the SASs using high-cadence high-resolution 131 Å images from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. Results. By identifying each individual spike during the decay phase of the selected eruptive flares, we found that the widths of spikes are log-normal distributed, while the Fourier power spectra of the overall supra-arcade EUV emission, including bright spikes and dark downflows as well as the diffuse background, are power-law distributed, in terms of either spatial frequency k or temporal frequency ν, which reflects the fragmentation of the VCS. We demonstrate that coronal emission-line intensity observations dominated by Kolmogorov turbulence would exhibit a power spectrum of E(k) ∼ k −13/3 or E(ν) ∼ ν −7/2 , which is consistent with our observations. By comparing the number of SASs and the turns of field lines as derived from the ICMEs, we found a consistent axial length of ∼ 3.5 AU for three events with a CME speed of ∼ 1000 km s −1 in the inner heliosphere, but a much longer axial length (∼ 8 AU) for the fourth event with an exceptionally fast CME speed of ∼ 1500 km s −1 , suggesting that this ICME is flattened and its 'nose' has well passed the Earth when the spacecraft traversed its leg.

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Velocities of Flare Kernels and the Mapping Norm of Field Line Connectivity

Cited by 17 publications

References 61 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

Observation of All Pre- and Post-reconnection Structures Involved in Three-dimensional Reconnection Geometries in Solar Eruptions

Investigation on the Spatiotemporal Structures of Supra-Arcade Spikes

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