Homologous Accelerated Electron Beams, a Quasiperiodic Fast-propagating Wave, and a Coronal Mass Ejection Observed in One Fan-spine Jet

Duan, Yadan; Shen, Yuandeng; Zhou, Xinping; Tang, Zehao; Zhou, Chen; Tan, Song

doi:10.3847/2041-8213/ac4df2

Cited by 22 publications

(25 citation statements)

References 67 publications

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“…As for quasiperiodic fast-propagating (QFP) wave trains, Shen et al (2022) divided them into narrow and broad QFP types based on their different physical properties. The former is characterized as propagating coherent wave fronts along the coronal loops with a relatively narrow angular width and a small intensity amplitude (Liu et al 2011;Shen & Liu 2012c;Miao et al 2019;Zhou et al 2021;Duan et al 2022), while the latter propagates along the solar surface with a broad angular width and a relatively large intensity amplitude (Shen et al 2019). In comparison, the physical parameters of broad QFP wave trains are more similar to the typical single-pulsed EUV waves.…”

Section: Introductionmentioning

confidence: 99%

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Zhou¹,

Shen²,

Liu³

et al. 2022

ApJL

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Large-scale extreme-ultraviolet (EUV) waves are frequently observed as an accompanying phenomenon of flares and coronal mass ejections (CMEs). Previous studies mainly focused on EUV waves with single wave fronts that are generally thought to be driven by the lateral expansion of CMEs. Using high spatiotemporal resolution multi-angle imaging observations taken by the Solar Dynamics Observatory and the Solar Terrestrial Relations Observatory, we present the observation of a broad quasiperiodic fast-propagating (QFP) wave train composed of multiple wave fronts along the solar surface during the rising phase of a GOES M3.5 flare on 2011 February 24. The wave train transmitted through a lunate coronal hole (CH) with a speed of ∼840 ± 67 km s−1, and the wave fronts showed an intriguing refraction effect when they passed through the boundaries of the CH. Due to the lunate shape of the CH, the transmitted wave fronts from the north and south arms of the CH started to approach each other and finally collided, leading to a significant intensity enhancement at the collision site. This enhancement might hint at the occurrence of interference between the two transmitted wave trains. The estimated magnetosonic Mach number of the wave train is about 1.13, which indicates that the observed wave train was a weak shock. Period analysis reveals that the period of the wave train was ∼90 s, in good agreement with that of the accompanying flare. Based on our analysis results, we conclude that the broad QFP wave train was a large-amplitude fast-mode magnetosonic wave or a weak shock driven by some nonlinear energy release processes in the accompanying flare.

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Section: Introductionmentioning

confidence: 99%

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Zhou¹,

Shen²,

Liu³

et al. 2022

ApJL

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“…The bifurcation of solar jets has been reported in several previous studies (e.g., Alexander & Fletcher 1999;Shen et al 2012;Duan et al 2022), and such a phenomenon has several different explanations, for example, dynamic response to the rapid transport of twist along magnetic field (Canfield et al 1996), the development of instability such as Kelvin-Helmholtz Instability (Alexander & Fletcher 1999), and the uncoupling of the erupting filament's two legs in filamentdriven jets (Shen et al 2012). In the present observation, we propose that the bifurcation of the TJ's north arm can be explained by the magnetic flux rope model of the filament, where the filament and the hosting cavity are considered as two interconnecting elements of one flux rope system (Gibson & Fan 2006).…”

Section: Discussionmentioning

confidence: 79%

Stereoscopic diagnosing of a filament-cavity flux rope system by tracing the path of a two-sided-loop jet

Tan

Shen

Zhou

et al. 2022

Monthly Notices of the Royal Astronomical Society: Letters

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The fine magnetic structure is vitally important to understanding the formation, stabilization and eruption of solar filaments, but so far, it is still an open question yet to be resolved. Using stereoscopic observations taken by the Solar Dynamics Observatory and Solar TErrestrial RElations Obsevatory, we studied the generation mechanism of a two-sided-loop jet (TJ) and the ejection process of the jet plasma into the overlying filament-cavity system. We find that the generation of the two-sided-loop jet was due to the magnetic reconnection between an emerging flux loop and the overlying filament. The jet’s two arms ejected along the filament axis during the initial stage. Then, the north arm bifurcated into two parts at about 50 Mm from the reconnection site. After the bifurcation, the two bifurcated parts were along the filament axis and the cavity which hosted the filament, respectively. By tracing the ejecting plasma flows of the TJ inside the filament, we not only measured that the magnetic twist stored in the filament was at least 5π but also found that the fine magnetic structure of the filament-cavity flux rope system is in well agreement with the theoretical results of Magnetic flux rope models.

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“…Hence, there is no correlation between the flare magnitude and type III bursts. In other words, the production of type III bursts depends mainly on the magnetic topology instead of flare energy (Krucker et al 2011;Glesener et al 2012;Duan et al 2022).…”

Section: Relation With Type III Radio Burstsmentioning

confidence: 99%

“…In Figure 12(c), the proportions of CFs related to jets at various flare magnitudes are demonstrated, being 25%, 52%, 53%, and 50% for B-, C-, M-, and X-class flares, respectively. Therefore, there is no preference of jet production for CFs with larger magnitudes as well (Chae et al 1999;Shibata et al 2007;Duan et al 2022).…”

Section: Relation With Coronal Jetsmentioning

confidence: 99%

Statistical Analysis of Circular-ribbon Flares

Zhang

De-chao

et al. 2022

ApJS

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Circular-ribbon flares (CFs) are a special type of solar flares owing to their particular magnetic topology. In this paper, we conducted a comprehensive statistical analysis of 134 CFs from 2011 September to 2017 June, including 4 B-class, 82 C-class, 40 M-class, and 8 X-class flares. The flares were observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory spacecraft. The physical properties of CFs are derived, including the location, area (A CF), equivalent radius (r CF) assuming a semispherical fan dome, lifetime (τ CF), and peak soft X-ray (SXR) flux in 1–8 Å. It is found that all CFs are located in active regions, with the latitudes between −30° and 30°. The distributions of areas and lifetimes could be fitted with a lognormal function. There is a positive correlation between the lifetime and area. The peak SXR flux in 1–8 Å is well in accord with a power-law distribution with an index of −1.42. For the 134 CFs, 57% of them are accompanied by remote brightenings or ribbons. A positive correlation exists between the total length (L RB) and average distance (D RB) of remote brightenings. About 47% and 51% of the 134 CFs are related to type III radio bursts and jets, respectively. The association rates are independent of flare energies. About 38% of CFs are related to minifilament eruptions, and the association rates increase with flare classes. Only 28% of CFs are related to coronal mass ejections (CMEs), meaning that a majority of them are confined rather than eruptive events. There is a positive correlation between the CME speed and peak SXR flux in 1–8 Å, and faster CMEs tend to be wider.

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Homologous Accelerated Electron Beams, a Quasiperiodic Fast-propagating Wave, and a Coronal Mass Ejection Observed in One Fan-spine Jet

Cited by 22 publications

References 67 publications

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Observations of a Flare-ignited Broad Quasiperiodic Fast-propagating Wave Train

Stereoscopic diagnosing of a filament-cavity flux rope system by tracing the path of a two-sided-loop jet

Statistical Analysis of Circular-ribbon Flares

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