Circular-ribbon flares and the related activities

Zhang, Qingmin

doi:10.1007/s41614-024-00144-9

Cited by 7 publications

(3 citation statements)

References 416 publications

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“…These findings suggest that the counterpropagating QFP wave trains within closed coronal loops can generate a turbulent cascade capable of carrying substantial energy for heating the corona in low-corona magnetic structures. Generally, it was found that the narrow QFP wave trains appear in similar periodicities with the quasiperiodic pulsations (QPP; Liu et al 2011;Shen & Liu 2012;Yuan et al 2013;Li et al 2018;Zhou et al 2022a;Duan et al 2022) of the accompanying flare emissions commonly seen from radio to hard X-rays (Nakariakov & Melnikov 2009;Li et al 2015Li et al , 2020Li et al , 2021Zhang et al 2016;Zhang 2024). This result aligns with previous studies indicating that flares can produce nonthermal electrons, which are accountable for microwave and X-ray emissions.…”

Section: Introductionsupporting

confidence: 89%

Broad and Bidirectional Narrow Quasiperiodic Fast-propagating Wave Trains Associated with a Filament-driven Halo Coronal Mass Ejection on 2023 April 21

Zhou,

Shen,

Yan

et al. 2024

ApJ

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This paper presents three distinct wave trains that occurred on 2023 April 21: a broad quasiperiodic fast-propagating (QFP) wave train and bidirectional narrow QFP wave trains. The broad QFP wave train expands outward in a circular wave front, while bidirectional narrow QFP wave trains propagate in the northward and southward directions, respectively. The concurrent presence of the wave trains offers a remarkable opportunity to investigate their respective triggering mechanisms. Measurement shows that the speed of the broad QFP wave train is in the range of 300–1100 km s−1 in different propagating directions. There is a significant difference in the speed of the bidirectional narrow QFP wave trains: the southward propagation achieves 1400 km s−1, while the northward propagation only reaches about 550 km s−1 accompanied by a deceleration of about 1–2 km s−2. Using the wavelet analysis, we find that the periodicity of the propagating wave trains in the southward and northward directions closely matches the quasiperiodic pulsations exhibited by the flares. Based on these results, the narrow QFP wave trains were most likely excited by the intermittent energy release in the accompanying flare. In contrast, the broad QFP wave train had a tight relationship with the erupting filament, probably attributed to the unwinding motion of the erupting filament, or the leakage of the fast sausage wave train inside the filament body.

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Section: Introductionsupporting

confidence: 89%

Broad and Bidirectional Narrow Quasiperiodic Fast-propagating Wave Trains Associated with a Filament-driven Halo Coronal Mass Ejection on 2023 April 21

Zhou,

Shen,

Yan

et al. 2024

ApJ

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“…Moreover, double or even multiple periods were simultaneously observed in the time series of the same flare, which could be explained as the fundamental and second or multiple harmonics (Inglis & Nakariakov 2009;Li 2022). The QPPs feature could also be found in the circular-ribbon flare, and this type of flare often occurs in a complicated magnetic structure associated with a fan-spine topology (see Török et al 2009;Zhang 2024), resulting in various kinds of flare QPPs (e.g., Kashapova et al 2020;Altyntsev et al 2022;Ning et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Localizing Quasiperiodic Pulsations in Hard X-Ray, Microwave, and Lyα Emissions of an X6.4 Flare

Li,

Hong,

Hou

et al. 2024

ApJ

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We report the simultaneous observations of quasiperiodic pulsations (QPPs) in wavelengths of hard X-ray (HXR), microwave, Lyα, and ultraviolet (UV) emissions during the impulsive phase of an X6.4 flare on 2024 February 22 (SOL2024-02-22T22:08). The X6.4 flare shows three repetitive and successive pulsations in HXR and microwave wavebands, and they have an extremely large modulation depth. The onset of flare QPPs is almost simultaneous with the start of magnetic cancellation between positive and negative fields. The wavelet power spectra suggest the presence of double periods, which are centered at ∼200 and ∼95 s, respectively. The long-period QPP can also be detected in Lyα and UV wavebands at the flare area, and it could be observed in the adjacent sunspot. Our observations indicate that the flare QPPs are most likely triggered by accelerated electrons that are associated with periodic magnetic reconnections. The long period at ∼200 s is probably modulated by the slow magnetoacoustic wave originating from the neighboring sunspot, while the short period at ∼95 s could be regarded as its second harmonic mode.

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“…Considering the three-dimensional (3D) scenario, with the aid of magnetic field extrapolation techniques and high-resolution observations, an increasing number of studies revealed that the 3D magnetic configuration of the coronal jets is a fan-spine structure (Shen 2021). This structure is composed of a null point, a dome-shaped fan, and the inner (outer) spines located inside (outside) the fan, which is typically accompanied by a circular flare ribbon and an inner bright patch (e.g., Masson et al 2009;Wang & Liu 2012;Li et al 2017Li et al , 2018Shen et al 2019b;Hou et al 2019;Lee et al 2020;Duan et al 2022Duan et al , 2024Huang et al 2024;Zhang 2024). In a high-resolution MHD simulation, Wyper et al (2017Wyper et al ( , 2018 showed a breakout model (Antiochos et al 1999) for coronal jets in a 3D fan-spine structure involving small filaments.…”

Section: Introductionmentioning

confidence: 99%

On the Determining Physical Factor of Jet-related Coronal Mass Ejections’ Morphology in the High Corona

Duan,

Shen,

Tang

et al. 2024

ApJ

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A solar jet can often cause coronal mass ejections (CMEs) with different morphologies in the high corona, for example, jet-like CMEs, bubble-like CMEs, and so-called twin CMEs that include a pair of simultaneous jet-like and bubble-like CMEs. However, what determines the morphology of a jet-related CME is still an open question. Using high spatiotemporal resolution stereoscopic observations taken by the Solar Dynamics Observatory and the Solar Terrestrial Relations Observatory from 2010 October to 2012 December, we performed a statistical study of jet-related CMEs to study the potential physical factors that determine the morphology of CMEs in the outer corona. Our statistical sample includes 16 jet-related CME events of which seven are twin CME events and nine are jet-like narrow CMEs. We find that all CMEs in our sample were accompanied by filament-driven blowout jets and Type III radio bursts during their initial formation and involved magnetic reconnection between filament channels and the surrounding magnetic fields. Most of our cases occurred in a fan-spine magnetic configuration. Our study suggests that the bubble-like components of twin CMEs lacking an obvious core are related to the expansion of the closed-loop systems next to the fan-spine topology, while the jet-like component is from the coronal extension of the jet plasma along open fields. Based on the statistical results, we conclude that the morphology of jet-related CMEs in the high corona may be related to the filament length and the initial magnetic null point height of the fan-spine structures.

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Circular-ribbon flares and the related activities

Cited by 7 publications

References 416 publications

Broad and Bidirectional Narrow Quasiperiodic Fast-propagating Wave Trains Associated with a Filament-driven Halo Coronal Mass Ejection on 2023 April 21

Broad and Bidirectional Narrow Quasiperiodic Fast-propagating Wave Trains Associated with a Filament-driven Halo Coronal Mass Ejection on 2023 April 21

Localizing Quasiperiodic Pulsations in Hard X-Ray, Microwave, and Lyα Emissions of an X6.4 Flare

On the Determining Physical Factor of Jet-related Coronal Mass Ejections’ Morphology in the High Corona

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